# pdgfootnote

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FICEK 2017 look for spin-dependent interactions between electrons by comparing precision spectroscopic measurements in He4 with theoretical calculations. See their Fig. 1 for limits up to mass(A0) = 10 keV.


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LIU 2017A is analogous to AHMED 2009A. See their Fig. 9 for limits between 0.25 keV < mass(A0) < 20 keV.


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LIU 2017A look for solar axions produced from Compton, bremsstrahlung, atomic-recombination and deexcitation channels, and set a limit for mass(A0) < 1 keV.


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LUO 2017 use a recent measurement of the dipole-dipole interaction between two iron atoms at the nanometer scale and set a limit for mass(A0) < 1 keV. See their Fig. 3 for mass-dependent limits.


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CORSICO 2016 studied the cooling rate of the pulsating DA white dwarf L19-2 based on an asteroseismic model.


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YOON 2016 look for solar axions with the axio-electric effect in CsI(Tl) crystals and set a limit for mass(A0) < 1 keV.


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TERRANO 2015 used a torsion pendulum and rotating attractor with 20-pole electron-spin distributions. See their Fig. 4 for a mass-dependent limit up to mass(A0) = 500 mueV.


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ABE 2014F set limits on the axioelectric effect in the XMASS detector assuming the pseudoscalar constitutes all the local dark matter. See their Fig. 3 for limits between mass(A0) = 40 -- 120 keV.


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APRILE 2014B is analogous to AHMED 2009A. Their Fig. 7 was later found to be incorrect due to a bug in their code. See Fig. 1 in APRILE 2017B for the corrected limits.


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DERBIN 2014 is an update of DERBIN 2013 with a BGO scintillating bolometer. See their Fig. 3 for mass-dependent limits.


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MILLER-BERTOLAMI 2014 studied the impact of axion emission on white dwarf cooling in a self-consistent way.


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ARMENGAUD 2013 is similar to AALSETH 2011. See their Fig. 10 for limits between 3 keV < mass(A0)< 100 keV.


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ARMENGAUD 2013 is similar to DERBIN 2012, and take account of axio-recombination and axio-deexcitation effects. See their Fig. 12 for mass-dependent limits.


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BARTH 2013 search for solar axions produced by axion-electron coupling, and obtained the limit, g(A e e).G(A gamma gamma)< 8.1E-23 GeV**-1 at 95%CL.


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DERBIN 2013 looked for 5.5 MeV solar axions produced in p d -->He3 A0 in a BGO detector through the axioelectric effect. See their Fig. 4 for mass-dependent limits.


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HECKEL 2013 studied the influence of 2 or 4 stationary sources each containing 6.0E24 polarized electrons, on a rotating torsion pendulum containing 9.8E24 polarized electrons. See their Fig. 4 for mass-dependent limits.


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VIAUX 2013A constrain axion emission using the observed brightness of the tip of the red-giant branch in the globular cluster M5.


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CORSICO 2012 attributed the excessive cooling rate of the pulsating white dwarf R548 to emission of axions with g(Aee) ~= 4.8E-13.


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DERBIN 2012 look for solar axions with the axio-electric effect in a Si(Li) detector. The solar production is based on Compton and bremsstrahlung processes.


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AHMED 2009A assume keV-mass pseudoscalars are the local dark matter and constrain the axio-electric effect in the CDMS detector. See their Fig. 5 for mass-dependent limits.


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These experiments measured induced magnetization of a bulk material by the spin-dependent potential generated from other bulk material with aligned electron spins, where the magnetic field is shielded with superconductor. The sign of the limit set by CHUI 1993 is opposite to that of the axion-mediated dipole-dipole potential.


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These experiments used a torsion pendulum to measure the potential between two bulk matter objects where the spins are polarized but without a net magnetic field in either of them. The limits reflect the corrected sign of the dipole-dipole potential.


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WINELAND 1991 looked for an effect of bulk matter with aligned electron spins on atomic hyperfine splitting using nuclear magnetic resonance.


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ALONSO-GONZALEZ 2025 use Super-Kamiokade data to search for the diffuse flux of axion-like particles produced in galactic core-collapse supernovae via the interaction with protons in the detector, A0 p --> p gamma. They set bounds on axion-proton couplings between a minimum and maximum of 2E-5 -- 2E-4 up to axion masses of 70 MeV, see their Fig. 4. ALONSO-GONZALEZ 2025A details an erratum for this publication.


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ARIAS-ARAGON 2025 use Borexino data to search for axion-induced pair production and inverse Compton scattering due to the flux of 5.5 MeV axions from proton-deuteron fusion in the Sun. They constrain the combination of axion-electron and axion-nucleon couplings for mass(A0) ~< 1 MeV as shown in their Fig. 4.


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BASILICO 2025 use Borexino data to search for the flux of 5.5 MeV axions produced through proton-deuteron fusion in the Sun, which can lead to detectable signals in the detector through axion decay to two photons, Primakoff and Compton conversion to photons, and the liberation of electrons through the axio-electric effect. They set bounds on the product of the axion-electron and axion-nucleon couplings, and the product of the axion-photon and axion-nucleon couplings, for mass(A0) < 1 MeV.


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GENG 2025 use a public electron recoil dataset from the XENONnT collaboration to search for events caused by the flux of 14.4 keV axions produced in M1 transitions of Fe57 nuclei in the solar interior. They set limits on the product of the axion-photon and axion-nucleon couplings and the product of the axion-electron and axion-nucleon couplings for axion masses below 14.4 keV.


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WALTER 2025 report results from a demonstrator for the CASPEr-Gradient experiment, which in this case used proton nuclear magnetic resonance spectroscopy of methanol to search for axion-like particle dark matter coupled to protons. They are sensitive in a narrow window around an ALP mass of 5.576741 neV. See their Fig. 3 for mass-dependent limits.


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ZHANG 2025A set limits on dark matter axion-like particles coupled to nucleons in the 1E-24 -- 5E-21 eV mass range by reanalyzing data from a Helium-3/Xenon-129 comagnetometer experiment originally performed to test for Lorentz and CPT violations. See their Fig. 3 for mass-dependent limits.


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LELLA 2024 update constraints on the axion-proton coupling from supernova 1987A based on the SN cooling argument (including a treatment of the trapping regime) as well as the non-observation of any coincident axion-induced events in the Kamiokande II neutrino detector. They exclude QCD axion models above 0.01 eV, and axion-like particles in a window that extends up to 300 MeV. See their Fig. 3 for mass-dependent limits.


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SU 2024 search for an axion-mediated dipole-dipole force between two separated spin-polarized samples of Xe129 gas. They set limits on the axion-neutron coupling for axion masses between 3.2 and 24.3 mueV. See their Fig. 4(b) for mass-dependent limits.


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KARANTH 2023 utilized an in-plane polarized deuteron beam in a storage ring to constrain the  axion-induced oscillating EDM of the deuteron for mass(A0) = 0.496 -- 0.502 neV. Assuming  axions account for all dark matter with rho_{{A}} ~= 0.55 GeV/cm**3, they derived  constraints on axion couplings to the deuteron EDM operator, gluons, and the deuteron spin. For  detailed limits, see their Figs. 19 -- 21.


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LEE 2023 analyzed data from a K-He3 comagnetometer, accounting for stochastic effects, to limit the axion-neutron coupling g(A n n) < 2.4E-10 GeV**-1 at 95% CL for mass(A0) = 0.4 -- 4 feV. They assumed axions form all dark matter with a density of 0.3 GeV/cm**3. See their Fig. 5 for the limits.


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BUSCHMANN 2022 studied the axion emission from five neutron stars with ages ~  E5 -- E6 years, comparing the simulation with axions to age and luminosity measurements. The mass bound assumes the KSVZ axion model with C(p) = -0.47 and C(n) = -0.02. See their Fig. 3 for the limits on the DFSZ axion model.


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GAVRILYUK 2022 look for solar axions from the ABC interactions with the experimental setup similar to GAVRILYUK 2015. The mass bound assumes the KSVZ axion model, S = 0.5, and mass(u)/mass(d) = 0.56.


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SCHULTHESS 2022 look for a time-oscillating neutron EDM caused by the coupling between axion dark matter and gluons, using a Ramsey-type apparatus for a cold neutron beam. See their Fig. 4 for limits in the range of mass(A0) = E-19 -- 4E-12 eV.


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AYBAS 2021 limits the axion couplings to the nucleon EDM and the nucleons as g(A N gamma) < 9.5E-4 GeV**-2 and g(A N N)/2mass(N) < 0.28 GeV**-1 (95 % CL) for mass(A0) = 162 -- 166 neV, based on a measurement of Pb207 solid-state NMR in a polarized ferroelecrtric crystal. Here mass(N) is the nucleon mass and g(A N N) is the dimensionless axion-nucleon coupling. They assume that axions make up all the dark matter with rho_{{A}} ~= 0.46 GeV/cm**3. See their Fig. 3 for the limits.


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BHUSAL 2021 looked for 5.5 MeV solar axions produced by p d --> He3 A0 through the axion-induced dissociation of deuterons by using SNO data, and set a limit on the isovector axion-nucleon coupling, |g**3(aN)| < 2E-5 GeV**-1, which is equivalent to |g(A n n) - g(A p p)| < 4E-5 in terms of the dimensionless axion-nucleon couplings.


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JIANG 2021 use the spin-amplifier based on hyperpolarized Xe129 gas to set limits on the axion couplings to nucleons as g(A N N)/2mass(N) < 3.2E-9 GeV**-1 (95 % CL) at mass(A0) = 52.94 feV, and comparable limits in the mass range of 8.3 -- 744 feV. Here mass(N) is the nucleon mass and g(A N N) is the dimensionless axion-nucleon coupling. They assume that axions make up all the dark matter with rho_{{A}} ~= 0.4 GeV/cm**3. See their Fig. 4b for the limits.


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ROUSSY 2021 look for a time-oscillating EDM of molecular ions HfF**+ induced by axion dark matter couplings to gluons. See their Fig. 3 for limits in the range of mass(A0) = E-22 -- E-15 eV.


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ZHANG 2021B use the gravitational waves from the binary neutron star inspiral GW170817 to  look for a type of axion whose mass is suppressed due to cancellation with additional  contributions. They exclude 1.6E16 < f(A) < E18 GeV at 3  sigma for mass(A0) ~< E-13 eV. See their Fig. 1 for mass-dependent limits.


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ABDELHAMEED 2020 look for the resonant excitation of Tm169 (8.41 keV) by solar axions produced via the Primakoff effect. The mass bound assumes the KSVZ axion model, S = 0.5, and mass(u)/mass(d) = 0.56. They set a limit on the product of axion couplings to photons and nucleons as G(A gamma gamma). g(A p p) < 1.44E-14 GeV**-1 (90 % CL).


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ABDELHAMEED 2020 look for the resonant excitation of Tm169 (8.41 keV) by solar axions produced via the axion-electron coupling. They set a limit on the product of axion couplings to electrons and nucleons as g(A e e ). g(A p p) < 2.81E-16 (90 % CL).


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APRILE 2020 look for solar axions from the ABC interactions, the Primakoff conversion, and the 14.4 keV M1 transition of Fe57. An excess is observed at low energies between 2 and 3 keV. See their Fig.8 for correlation between the couplings.


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KLIMCHITSKAYA 2020 use the measurement of the Casimir force between a Au-coated microsphere and a SiC plate to constrain the force due to two-axion exchange for 17.8 < mass(A0) < 100 eV. See their Fig. 2 for mass-dependent limits.


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WANG 2020A is an update of LIU 2017A. The limit assumes the DFSZ axion. See their Fig. 7 for the limit on product of axion couplings to electrons and nucleons.


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LEINSON 2019 is analogous to BEZNOGOV 2018, but estimating the axion luminosity based on the Tolman's analytic solution to the Einstein equations of spherical fluids in hydrostatic equilibrium. The dimensionless axion-neutron coupling is constrained as g(Ann) < 1.0E-10.


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LLOYD 2019 is analogous to BERENJI 2016. They highlight that the limit obtained with this technique strongly depends on the assumed NS core temperature.


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SMORRA 2019 look for spin-precession effects from ultra-light axion dark matter in the pbar spin-flip resonance data. Assuming rho_{{A}} = 0.4 GeV/cm**3, they constrain the dimensionless axion-antiproton coupling as g(A pbar pbar) < 2 -- 9 at 95% CL for mass(A0) = 2E-23 -- 4E-17 eV. See the right panel of their Fig. 3.


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WU 2019 look for axion-induced time-oscillating features of the NMR spectrum of acetonitrile-2-C13. Assuming C(p) = C(n) and rho_{{A}} = 0.4 GeV/cm**3, they constrain the dimensionless axion-nucleon coupling as g_{{ANN}} < 6E-5 for mass(A0) = E-21 -- 1.3E-17 eV. Note that the limits for mass(A0) < E-21 eV in their Fig. 3(a) should be weaker than those for heavier masses. See ADELBERGER 2019 and WU 2019C on this issue.


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ARMENGAUD 2018 is analogous to ALESSANDRIA 2013. The quoted limit assumes the DFSZ axion model. See their Fig. 4 for the limit on product of axion couplings to electrons and nucleons.


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BEZNOGOV 2018 constrain the axion-neutron coupling by assuming that thermal evolution of the hot neutron star HESS J1731-347 is dominated by the lowest possible neutrino emission. The quoted limit assumes the KSVZ axion with the effective Peccei-Quinn charge of the neutron C(n) = -0.02. The dimensionless axion-neutron couling is constrained as g(Ann) < 2.8E-10.


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GAVRILYUK 2018 look for the resonant excitation of Kr83 (9.4 keV) by solar axions produced via the Primakoff effect. The mass bound assumes mass(u)/mass(d) = 0.56 and S = 0.5.


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HAMAGUCHI 2018 studied the axion emission from the neutron star in Cassiopeia A based on the minimal cooling scenario which explains the observed rapid cooling rate. The quoted limit corresponds to f(A) > 5E8 GeV obtained for the KSVZ axion with C(p) = -0.47 and C(n) = -0.02.


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ABEL 2017 look for a time-oscillating neutron EDM and an axion-wind spin-precession effect respectively induced by axion dark matter couplings to gluons and nucleons. See their Fig. 4 for limits in the range of mass(A0) = E-24 -- E-17 eV.


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ABGRALL 2017 limit assumes the hadronic axion model used in ALESSANDRIA 2013. See their Fig. 4 for the limit on product of axion couplings to electrons and nucleons.


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FU 2017A look for the 14.4 keV Fe57 solar axions. The limit assumes the DFSZ axion model. See their Fig. 3 for mass-dependent limits on the axion-electron coupling. Notice that in this figure the DFSZ and KSVZ lines should be interchanged.


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KLIMCHITSKAYA 2017A use the differential measurement of the Casimir force between a Ni-coated sphere and Au and Ni sectors of the structured disc to constrain the axion coupling to nucleons for 2.61 meV < mass(A0) < 0.9 eV. See their Figs. 1 and 2 for mass dependent limits.


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LIU 2017 is analogous to ALESSANDRIA 2013. The limit assumes the hadronic axion model. See their Fig. 6(b) for the limit on product of axion couplings to electrons and nucleons.


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BERENJI 2016 used the Fermi LAT observations of neutron stars to look for photons from axion decay. They assume the effective Peccei-Quinn charge of the neutron C(n) = 0.1 and a neutron-star core temperature of 20 MeV.


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GAVRILYUK 2015 look for solar axions emitted by the M1 transition of Kr83 (9.4 keV). The mass bound assumes mass(u)/mass(d) = 0.56 and S = 0.5.


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KLIMCHITSKAYA 2015 use the measurement of differential forces between a test mass and  rotating source masses of Au and Si to constrain the force due to two-axion  exchange for 1.7E-3 < mass(A0) < 0.9 eV. See their Figs. 1 and 2 for mass dependent limits.


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BEZERRA 2014 use the measurement of the thermal Casimir-Polder force between a Bose-Einstein condensate of Rb87 atoms and a SiO(2) plate to constrain the force mediated by exchange of two pseudoscalars for 0.1 meV < mass(A0)< 0.3 eV. See their Fig. 2 for the mass-dependent limit on pseudoscalar coupling to nucleons.


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BEZERRA 2014A is analogous to BEZERRA 2014. They use the measurement of the Casimir pressure between two Au-coated plates to constrain pseudoscalar coupling to nucleons for 1E-3 eV < mass(A0)< 15 eV. See their Figs. 1 and 2 for the mass-dependent limit.


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BEZERRA 2014B is analogous to BEZERRA 2014. BEZERRA 2014B use the measurement of the normal and lateral Casimir forces between sinusoidally corrugated surfaces of a sphere and a plate to constrain pseudoscalar coupling to nucleons for 1 eV < mass(A0) < 20 eV. See their Figs. 1 -- 3 for mass-dependent limits.


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BEZERRA 2014C is analogous to BEZERRA 2014. They use the measurement of the gradient of the Casimir force between Au- and Ni-coated surfaces of a sphere and a plate to constrain pseudoscalar coupling to nucleons for 3E-5 eV < mass(A_{{0}}()) < 1 eV. See their Figs. 1, 3, and 4 for the mass-dependent limits.


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BLUM 2014 studied effects of an oscillating strong CP phase induced by axion dark matter on the primordial He4 abundance. See their Fig. 1 for mass-dependent limits.


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LEINSON 2014 attributes the excessive cooling rate of the neutron star in Cassiopeia A to axion emission from the superfluid core, and found C(n)**2 mass**2(A0) ~= 5.7E-6 eV**2, where C(n) is the effective Peccei-Quinn charge of the neutron.


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ALESSANDRIA 2013 used the CUORE experiment to look for 14.4 keV solar axions produced from the M1 transition of thermally excited Fe57 nuclei in the solar core, using the axio-electric effect. The limit assumes the hadronic axion model. See their Fig. 4 for the limit on product of axion couplings to electrons and nucleons.


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ARMENGAUD 2013 is analogous to ALESSANDRIA 2013. The limit assumes the hadronic axion model. See their Fig. 8 for the limit on product of axion couplings to electrons and nucleons.


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BELLI 2012 looked for solar axions emitted by the M1 transition of Li7*** (478 keV) after the electron capture of Be7, using the resonant excitation Li7 in the LiF crystal. The mass bound assumes mass(u)/mass(d) = 0.55, mass(u)/mass(s) = 0.029, and the flavor-singlet axial vector matrix element S = 0.4.


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BELLINI 2012B looked for 5.5 MeV solar axions produced in the p d --> He3 A0.The limit assumes the hadronic axion model. See their Figs. 6 and 7 for mass-dependent limits on productsof axion couplings to photons, electrons, and nucleons.


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DERBIN 2011 looked for solar axions emitted by the M1 transition of thermally excited Fe57 nuclei in the Sun, using their possible resonant capture on Fe57 in the laboratory. The mass bound assumes mass(u)/mass(d) = 0.56 and the flavor-singlet axial vector matrix element S = 3F-D ~= 0.5.


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BELLINI 2008 consider solar axions emitted in the M1 transition of Li7*** (478 keV) and look for a peak at 478 keV in the energy spectra of the Counting Test Facility (CTF), a Borexino prototype. For mass(A0) < 450 keV they find mass-dependent limits on products of axion couplings to photons, electrons, and nucleons.


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ADELBERGER 2007 use precision tests of Newton's law to constrain a force contribution from the exchange of two pseudoscalars. See their Fig. 5 for limits on the pseudoscalar coupling to nucleons, relevant for mass(A0) below about 1 meV.


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AYRES 2023 at PSI use their neutron EDM setup to look for a mm to micron-range spin-dependent force between ultracold spin-polarized neutrons stored in vacuum and the unpolarised nucleons in the surrounding apparatus. They constrain a nucleon-neutron monopole-dipole interaction parameterised by the coupling g_s^N g_p^n. They set a limit of g_{{s}}^Ng_{{p}}^n < E-20 (95% CL) for a 1 meV mass axion, see Fig. 6.


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PODDAR 2023 search for long-range monopole-dipole forces between the polarized population of electrons inside the Earth and the unpolarised nucleons in the Sun, which would affect the precession of orbital perihelion. However, the most competitive limit is obtained by combining the monopole-monopole force constraints on g^N_s from planetary precession with the strongest stellar bound on the pseudoscalar electron coupling (g^e_p), shown in Fig. 5.


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ZHANG 2023 look for changes of the ratio of precession frequencies between Xe129 and Xe131 as the bias field is flipped in Earth's gravitational field after Earth roation effect is subtracted. They find g_{{p}}^ng_{{s}}^N < 1E-26 -- 3.7E-36 for lambda = 0.3 -- 1E10 m. See their Fig. 4 for limits as a function of lambda.


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CRESCINI 2022 is an update of CRESCINI 2017, and find g_{{p}}^eg_{{s}}^N <=  5.7E-32 and g_{{p}}^eg_{{s}}^e <= 1.6E-31 for lambda ~> 10 cm at  95% CL. See their Fig. 4 for limits as a function of lambda.


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FENG 2022 look for changes of the ratio of precession frequencies between Xe129  and Xe131 when a BGO crystal is positioned near the atomic cell. They find  g_{{p}}^ng_{{s}}^N < 2E-20 -- 3E-24 for lambda = 0.11 -- 0.55 mm. See  their Fig. 4 for limits as a function of lambda.


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AFACH 2021 look for axion domain walls coupled to atomic spins by using the global network of  optical magnetometers. Assuming that the axion domain walls make up all dark matter, they exclude  the effective decay constant below 4E5 GeV for mass(A0) in the range of E-15 -- E-11  eV. See their Fig. 4 for the mass-dependent limits.


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DZUBA 2018 used atomic EDM measurements to derive limits on the product of the pseudoscalar coupling to nucleon and the scalar coupling to electron, which improved on the laboratory bounds for mass(A0) > 0.01 eV. See their Fig. 1 for mass-dependent limits.


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STADNIK 2018 used atomic and molecular EDM experiments to derive limits on the product of the pseudoscalar couplings to electron and the scalar coupling to nucleon and electron. See their Fig. 2 for mass-dependent limits, which improved on the laboratory bounds for mass(A0) > 0.01 eV.


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CRESCINI 2017 use the QUAX-g_{{p}}g_{{s}} experiment to look for variation of a paramagnetic GSO crystal magnetization when rotating lead disks are positioned near the crystal, and find g = g_{{p}}^eg_{{s}}^N < 4.3E-30 for lambda = 0.1 -- 0.2 m at 95% CL. See their Fig. 6 for limits as a function of lambda.


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AFACH 2015 look for a change of spin precession frequency of ultracold neutrons when a magnetic field with opposite directions is applied, and find g < 2.2E-27 (m/lambda)**2 at 95% CL for 1 mum < lambda < 5 mm. See their Fig.  3 for their limits.


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STADNIK 2015 studied proton and neutron spin contributions for nuclei and derive the limits g < E-28 -- E-23 for lambda > 3E-4 m using the data of TULLNEY 2013. See their Figs. 1 and 2 for lambda-dependent limits.


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TERRANO 2015 used a torsion pendulum and rotating attractor, and derived a restrictive limit on the product of the pseudoscalar coupling to electron and the scalar coupling to nucleons,  g < 9E-29 -- 5E-26 for mass(A0) < 1.5 -- 400 mueV. See their Fig. 5 for mass-dependent limits.


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BULATOWICZ 2013 looked for NMR frequency shifts in polarized Xe129 and Xe131 when a zirconia rod is positioned near the NMR cell, and find g < 1E-19 -- 1E-24 for lambda = 0.01 -- 1 cm. See their Fig. 4 for their limits.


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CHU 2013 look for a shift of the spin precession frequency of polarized He3 in the presence of an unpolarized mass, in analogy to YOUDIN 1996. See Fig. 3 for limits on g in the approximate mass(A0) range 0.02 -- 2 meV.


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TULLNEY 2013 look for a shift of the precession frequency difference between the colocated He3 and Xe129 in the presence an unpolarized mass, and derive limits g < 3E-29 -- 2E-22 for lambda > 3E-4 m. See their Fig. 3 for lambda-dependent limits.


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RAFFELT 2012 show that the pseudoscalar couplings to electron and nucleon and the scalar coupling to nucleon are individually constrained by stellar energy-loss arguments and searches for anomalous monopole-monopole forces, together providing restrictive constraints on g. See their Figs. 2 and 3 for results.


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HOEDL 2011 use a novel torsion pendulum to study the force by the polarized electrons of an external magnet. In their Fig. 3 they show restrictive limits on g in the approximate mass(A0) range 0.03 -- 10 meV.


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PETUKHOV 2010 use spin relaxation of polarized He3 and find g < 3E-23 (cm/lambda)**2 at 95% CL for the force range lambda = E-4 -- 1 cm.


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SEREBROV 2010 use spin precession of ultracold neutrons close to bulk matter and find g < 2E-21 (cm/lambda)**2 at 95% CL for the force range lambda = E-4 -- 1 cm.


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IGNATOVICH 2009 use data on depolarization of ultracold neutrons in material traps. They show lambda-dependent limits in their Fig. 1.


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SEREBROV 2009 uses data on depolarization of ultracold neutrons stored in material traps and finds g<2.96E-21 (cm/lambda)**2 for the force range lambda = E-3 -- 1 cm and g<3.9E-22 (cm/lambda)**2 for lambda = E-4 -- E-3 cm, each time at 95% CL, significantly improving on BAESSLER 2007.


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BAESSLER 2007 use the observation of quantum states of ultracold neutrons in the Earth's gravitational field to constrain g for an interaction range 1 mum-a few mm. See their Fig. 3 for results.


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HECKEL 2006 studied the influence of unpolarized bulk matter, including the laboratory's surroundings or the Sun, on a torsion pendulum containing about 9E22 polarized electrons. See their Fig. 4 for limits on g as a function of interaction range.


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NI 1999 searched for a T-violating medium-range force acting on paramagnetic Tb F(3) salt. See their Fig. 1 for the result.


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POSPELOV 1998 studied the possible contribution of T-violating Medium-Range Force to the neutron electric dipole moment, which is possible when axion interactions violate CP. The size of the force among nucleons must be smaller than gravity by a factor of 2E-10 (1 cm/lambda(A)), where lambda(A)=hbar/mass(A)c.


pdgid: S029IAT
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YOUDIN 1996 compared the precession frequencies of atomic Hg199 and Cs when a large mass is positioned near the cells, relative to an applied magnetic field. See Fig. 3 for their limits.


pdgid: S029IAT
text:
RITTER 1993 studied the influence of bulk mass with polarized electrons on an unpolarized torsion pendulum, providing limits in the interaction range from 1 to 100 cm.


pdgid: S029IAT
text:
VENEMA 1992 looked for an effect of Earth's gravity on nuclear spin-precession frequencies of Hg199 and Hg201 atoms.


pdgid: S029IAT
text:
WINELAND 1991 looked for an effect of bulk matter with aligned electron spins on atomic hyperfine resonances in stored Be9**+ ions using nuclear magnetic resonance.


pdgid: S029HPH
text:
ABLIKIM 2025CL search for kinetically mixed dark photons using the BESIII detector. They use the sample J/psi events collected to measure the transition form factor of the eta meson. Limits are derived on the branching ratio for eta --> gamma gamma^', gamma^' --> e+ e- and presented in terms of mass-dependent limits on the kinetic mixing parameter in Fig. 7.


pdgid: S029HPH
text:
ALBAKRY 2025 report a search with the SuperCDMS detector for hidden photon dark matter absorption on silicon. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
AN 2025 search for dark photon dark matter resonantly converting into photons in the solar corona plasma, leading a signal detectable by the STEREO and Parker Solar Probe spacecraft. See their Fig. 2 for mass-dependent limits.


pdgid: S029HPH
text:
ANDREEV 2025 present the first hidden photon limits from the NA64e experiment using a 70 GeV positron beam. They set constraints on an invisibly decaying hidden photon that kinetically mixes with the photon. See Fig. 14 for various mass-dependent limits, noting the assumed parameter values for the dark gauge coupling and dark matter mass.


pdgid: S029HPH
text:
APRILE 2025A present results from a search with XENONnT for dark photon dark matter absorption on electrons in liquid xenon. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
ASWATHI 2025 use LIGO-VIRGO-KAGRA data from the black hole binary merger events GW231123 and GW190517 to search for evidence of the superradiant build-up of a cloud of vector bosons, which could act to spin down the black holes. They set lower limits on the dark photon kinetic mixing and present mass-dependent limits in Fig. 2.


pdgid: S029HPH
text:
BAUDIS 2025 presents results from the QROCODILE experiment which uses a superconducting nanowire single photon detector to search for low-mass dark matter. Fig. 2 shows mass-dependent constraints on hidden photon absorption.


pdgid: S029HPH
text:
BLOCH 2025 present results from a search for single-electron events in the SENSEI low-mass dark matter detector. See their Fig. 4 for mass-dependent limits on dark photon absorption.


pdgid: S029HPH
text:
CAPUTO 2025 present a new bound on dark photon emission from core-collapse supernovae. They consider the cooling effect of resonant dark photon production behind the shock wave which, if too excessive, can potentially prevent the explosion. In the case of SN1987A, this consideration supersedes the standard supernova cooling argument and leads to a bound that is strongest in the sub-MeV mass region. See their Fig. 2 for mass-dependent limits.


pdgid: S029HPH
text:
CHOI 2025 place bounds on a dark matter model using the NEON reactor neutrino experiment. They explore a scenario in which the high flux of photons from the nuclear reactor leads to a flux of dark photons; those dark photons can then decay into dark matter particles in the detector that scatter on electrons. See their Fig. 3 for mass-dependent bounds on the dark photon mediator, obtained for the dark matter mass mass(gamma^')/3 and the hidden gauge coupling alpha(D) = 0.1.


pdgid: S029HPH
text:
CORTINA-GIL 2025A search for kinetically mixed hidden photons decaying to hadronic final states in the NA62 beam dump. Quoted limit applies around 0.8 GeV, but does not extend to arbitrarily large kinetic mixing. See their Fig. 7 for mass-dependent limits combining this hadronic analysis and the dilepton channel reported in CORTINA-GIL 2024A.


pdgid: S029HPH
text:
CORTINA-GIL 2025B report limits on an invisibly decaying dark photon produced in the decays of K+ and pi0 in the NA62 detector. See their Fig. 8 for mass-dependent limits.


pdgid: S029HPH
text:
EGGE 2025 search for dark photon dark matter using the prototype setup of the MADMAX dielectric disk haloscope. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
LI 2025 search for MeV-mass dark photons making up the dark matter halo of the galaxy that could be absorbed by liquid xenon in the PandaX detector. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. The quoted limit is at mass(gamma^') = 150 keV. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
LINDEN 2025 extend limits on dark photons as a dark matter candidate at masses below the electron pair creation threshold. They search for evidence of dark photon-to-three-photon decays using data from the INTEGRAL space telescope. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
MELO-GALINDO 2025 search for evidence of mixing between standard model and dark photons imprinted on the TeV gamma-ray spectra of the Crab Nebula and gamma-ray source MGRO J1908+06, using data from HAWC and LHAASO. See their Figs. 3 -- 6 for mass-dependent limits for both sources and under various model assumptions.


pdgid: S029HPH
text:
MIRASOLA 2025 search for evidence of superradiant clouds of dark photons surrounding black holes, which are expected to produce pulsating radio emissions, and continuous gravitational wave signals that could be observed by LIGO-Virgo-KAGRA. Their bound disfavours dark photons within a specific range of masses and kinetic mixing parameters between E-9 -- E-7, subject to uncertainties about the black hole population and details about the cloud's radio emission. See their Fig. 5.


pdgid: S029HPH
text:
ROMERO-JORGE 2025 set limits on kinetically-mixed dark photons produced through various decays in heavy-ion collisions and then decaying to dileptons. They incorporate a range of heavy ion data from across the SIS, RHIC and LHC. They present various mass-dependent limits in their Fig. 7 for different choices for the dark photon "surplus" - the maximum permissible increase in a dilepton yield from dark photons compared to the Standard Model yield.


pdgid: S029HPH
text:
TROST 2025 use VLT/UVES observations of the quasar HE0940-1050 to search for resonant conversion of dark photon dark matter into photons, which would heat the intergalactic medium and imprint on the quasar's Lyman-alpha forest spectrum. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
ZENG 2025 place a bound on keV-scale dark photons making up the halo of the galaxy by searching for electron recoil events in the PandaX detector. See Fig. 3(f) for mass-dependent limits.


pdgid: S029HPH
text:
ZHAO 2025 use a flux-tunable resonant cavity to search for dark photon dark matter in a narrow frequency window around 5.69 GHz, performing microwave single photon detection using a transmon qubit. The quoted limit assumes a local dark matter density of rho(gamma^') = 0.45 GeV/cm**3


pdgid: S029HPH
text:
ZHAO 2025A use a single-site, two-sensor array of commercial scalar optically pumped magnetometers to search for dark photon dark matter converting into photons. The relevant observable signal appears in this low-mass regime due to the action of the Earth's ionosphere as transducer. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
AAD 2024AS search for hidden photons resulting from Higgs decays in the Falkowski-Ruderman-Volansky-Zupan model. See Fig. 7 for mass-dependent limits, value shown taken from the most constraining point at 10 GeV mass. The limits do not extend to arbitrarily high values of the kinetic mixing, stopping between E-4 and E-7 at the lower and upper end of the mass range respectively. The limit is also dependent on the branching fraction for Higgs decays resulting in dark photons.


pdgid: S029HPH
text:
ABRATENKO 2024A search for dark trident scattering at a neutrino beam using the MicroBooNE detector. Events involve a pair of particles chi chibar produced from pi0 or eta decays mediated by a dark photon, these particles then scatter off Argon in the detector and can produce an additional dark photon which then decays. See Fig. 7 for mass-dependent limits under three possible scenarios for the chi particle.


pdgid: S029HPH
text:
ABREU 2024 look for hidden photons produced from the p p collision in the decay channel gamma^' --> e+ e-, and exclude at 90% CL the region of chi = 4E-6 -- 2E-4 and mass(gamma^') = 10 -- 80 MeV, with the newly excluded region near the higher values of chi. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
ADACHI 2024C follows KOTAKA 2023 of the DOSUE-RR collaboration, searching for hidden photon dark matter conversion using a millimetre-wave receiver and a radioshielding box. See Fig. 11 for mass dependent limits.


pdgid: S029HPH
text:
AGOSTINI 2024A report a search for dark photon dark matter absorption and dark Compton scattering on germanium, generating electron events in the GERDA experiment. The quoted limit is at mass(A0) = 150 keV. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
AGRAWAL 2024 search for hidden photon dark matter via stimulated emission of a photon from a microwave cavity prepared in a non-classical state by a superconducting qubit.


pdgid: S029HPH
text:
ANDREEV 2024A perform a missing-energy search in the NA64 detector to look for an MeV-scale hidden photon mediator to a stable fermionic dark sector particle. See Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
ANDREEV 2024E report results from the NA64mu beam dump experiment, employing a high-intensity muon beam. They set limits on the kinetic mixing parameter of an invisibly decaying hidden photon. See their Fig. 19 for mass-dependent limits.


pdgid: S029HPH
text:
ARAMBURO-GARCIA 2024 search for evidence of resonant conversion of regular photons into dark photons within the inter-galactic medium using the expected imprint on the CMB anisotropies. Quoted limit is for their "conservative" approach - see their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
ARNQUIST 2024 use the MAJORANA DEMONSTRATOR to search for keV-mass hidden photon dark matter absorption by Germanium. See Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
CERVANTES 2024 use a superconducting radio frequency cavity at the SQMS Centre (Fermilab) to search for hidden photon dark matter at 1.3 GHz. See their Fig. 3 for limits in context.


pdgid: S029HPH
text:
CORTINA-GIL 2024A report results from the NA62 beam dump experiment, searching for production and decays of dark photons to lepton pairs. Quoted limit applies around 300 MeV, but does not extend to arbitrarily high kinetic mixing. See their Fig. 4 for mass-dependent limits


pdgid: S029HPH
text:
DOLAN 2024 constrain anomalous cooling of globular cluster stars due to the emission of hidden photons. Best limit is taken from the envelope of limits from the R parameter, R2 parameter and Tip of the Red Giant branch. This study includes hidden photon emission in stellar evolution simulation and so supersedes red giant bound in AN 2020.


pdgid: S029HPH
text:
HE 2024 present results from the APEX collaboration. They look for hidden photon dark matter using a radio frequency cavity at 7.139 GHz. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
KNIRCK 2024 search for hidden photon dark matter using GigaBREAD, a broadband haloscope operating at room temperature that uses a parabolic reflector and a horn antenna. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
LEVINE 2024 search for hidden photon dark matter using Dark E-Field Radio, a broadband haloscope consisting of an E-field antenna inside a shielded room. This is a continuation of their experiment previously reported in GODFREY 2021. See their Fig. 12 for mass-dependent limits.


pdgid: S029HPH
text:
LIU 2024 constrain hidden photon dark matter over a broad mass range using the very high-energy gamma-ray spectrum of blazars Mrk 501 and Mrk 421. See their Fig. 4 for mass-dependent limits which also depend on the density profiles of the host halos of the blazars. Quoted limit is for the case where the host halos have an NFW profile in Fig. 6.


pdgid: S029HPH
text:
MCCARTHY 2024 search for evidence of photons converting into hidden photons as they traverse large-scale structure, which would lead to a patchy-screening effect observable in CMB anisotropy maps. See their Fig. 3 for mass-dependent limits. This analysis improves upon a similar study by ARAMBURO-GARCIA 2024 - see the note added in MCCARTHY 2024.


pdgid: S029HPH
text:
TANG 2024 present results from a hidden photon dark matter search at 1.3 GHz with SHANHE, a tunable superconducting radio frequency cavity. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
YAN 2024A use data from the JUNO probe to constrain hidden photons via the way they would modify Jupiter's magnetic field. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
AAD 2023BO look for rare decays of the Z boson, Z --> gamma^' + H^', with dark Higgs decaying into a pair of hidden photons, assuming that at least two of the hidden photons decay into e+ e- or mu+ mu-. The quoted limit assumes the hidden fine structure constant alpha_{{D}} = 0.1 and the dark Higgs mass ranging 20 to 70 GeV. See their Fig.5 for the mass-dependent limits.


pdgid: S029HPH
text:
AAD 2023I look for exotic decays of the SM-like Higgs boson, H --> gamma^' gamma^' with hidden photons decaying into displaced lepton or light quark pairs, and set limits on the kinetic mixing within 1E-4 -- 1E-8 for the given mass range. The quoted limit is for mass(A0) ~= 13 GeV with a branching fraction of 0.1 for the Higgs decaying into hidden photon pairs. See their Fig. 13 for the mass-dependent limits.


pdgid: S029HPH
text:
AAD 2023T is analogous to AAD 2022S, but using the Z H production mode, and set  the upper limit on the branching ratio B(H --> gamma gamma^') within 0.0219 -- 0.0252   (95% CL).


pdgid: S029HPH
text:
AALBERS 2023A look for an absorption of hidden photon dark matter. The quoted limit is for mass(gamma^') = 1.4 keV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
ABLIKIM 2023AF look for invisible decays of hidden photons produced in the reaction e+ e- --> gamma gamma^'. They set limits within the 1.6E-3 -- 5.7E-3. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
ABUDINEN 2023B look for hidden photons in the dark Higgsstrahlung process, e+ e- --> gamma^' H^'  (gamma^' --> mu+ mu-) with H^' being invisible. They set upper limits on the product of the kinetic mixing and the hidden gauge coupling, chi^2.alpha_{{D}}, in the range of 1.7E-8 -- 2E-6 at 90% CL for a 1 GeV dark Higgs mass. See their Fig. 3 for the mass-dependent limits.


pdgid: S029HPH
text:
ADHIKARI 2023 look for the annual modulation signal induced by solar flux of hidden photons. See their Fig. 10 for mass-dependent limits.


pdgid: S029HPH
text:
ADHIKARI 2023A look for absorption and Compton-like processes of hidden photon dark matter.  The quoted limit is for mass(gamma^') ~= 12 keV. Limits between 6E-14 -- 3E-11 are  obtained. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
ADRIAN 2023 is an update of ADRIAN 2018, and use the data from the 2016 engineering run  at 2.3 GeV. The quoted limit is at mass(gamma^') ~= 74 MeV. See their Fig. 28 for the  mass-dependent limits.


pdgid: S029HPH
text:
AGNES 2023A look for an absorption of hidden photon dark matter. The quoted limit is for  mass(gamma^') = 0.03 keV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 2 for mass-dependent limits.


pdgid: S029HPH
text:
AN 2023A look for absorption of hidden photon dark matter at radio telescopes, setting limits based on data from the FAST telescope. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 1 for mass-dependent limits.


pdgid: S029HPH
text:
ANDREEV 2023 is an update of ANDREEV 2021 and ANDREEV 2021A. The quoted limit applies to mass(gamma^') = 1 MeV. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
BAJJALI 2023 look for hidden photon dark matter by using a 12 -- 18 GHz dish antenna at U. Hamburg that is sensitive to vertically aligned hidden photon polarizations. They assume a local density of rho(gamma^') = 0.3 GeV/cm**3. See their Figure 12 for mass-dependent limits in the range of mass(gamma^') = 50 -- 75 mueV under the assumption of randomly aligned hidden photon polarizations, defined as "1 sigma sensitivity". The run is labelled BRASS-p.


pdgid: S029HPH
text:
CORTINA-GIL 2023C NA62 beam dump experiment searches for hidden photons decaying to mu+ mu-, extending their previous search CORTINA-GIL 2019. The quoted limit applies at 300 MeV but does not extend to arbitrarily large kinetic mixing parameters. See Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
HAYRAPETYAN 2023G search for kinetically mixed hidden photons in proton-proton collisions at the LHC that would generate a narrow peak in the mass spectrum of dimuon events. The mass window between 2.6 and 4.2 GeV is left unconstrained to avoid J/psi and psi(2S) resonances. Mass dependent limits given in their Fig. 6.


pdgid: S029HPH
text:
KOTAKA 2023 is an update of TOMITA 2020, and set limits chi < 0.3 -- 2E-10 for the quoted mass range. The local density rho(gamma^') = 0.39 GeV/cm**3 is assumed. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
LI 2023I set cooling bounds on the emission of hidden photons from the Sun, red giant, and horizontal branch stars, including emission of both the transverse and longitudinal modes. Cooling bounds are computed assuming a static model as opposed to considering the impact on stellar evolution. The result is comparable to earlier estimates of the same bound e.g. REDONDO 2013. Limit applies at the most constraining mass around 200 eV for the solar bound.


pdgid: S029HPH
text:
RAMANATHAN 2023 look for hidden photon dark matter using a gold-plated copper dish antenna cooled to 20 mK. The local density rho(gamma^') = 0.45 GeV/cm**3 is assumed. Limits between 7.9E-13 and 3.81E-12 are obtained. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
ROMANENKO 2023 employed two superconducting radio frequency cavities with a high quality factor, optimized for detecting the longitudinal polarization of the hidden photon. The quoted limit is set at mass(gamma^') ~= 5mueV. See their Fig. 4 for the mass-dependent limits.


pdgid: S029HPH
text:
XIA 2023 is analogous to WU 2022A and use the Fermi-LAT pulsar timing array. They set a bound on the local density as rho(gamma^') ~< 7 GeV/cm**3 for  mass(gamma^')  ~< E-23 eV at 95% CL, with weaker constraints up to E-22 eV.  See their Fig. 1  for the mass-dependent limits.


pdgid: S029HPH
text:
AAD 2022J look for exotic decays of the SM-like Higgs boson, H --> gamma^' gamma^' --> 4 lepton and  H --> Z gamma^' --> 4 lepton,  and set limits on the kinetic mixing and the Higgs portal  coupling. See their Figs. 19 and 20 for the mass-dependent limits.


pdgid: S029HPH
text:
AAD 2022S look for decays of a Higgs boson into gamma and gamma^' using the VBF production mode, and set the upper limit on the branching ratio at 0.018 (95% CL) for the 125 GeV Higgs boson. For the quoted mass range, the signal acceptance changes by less than 1%.


pdgid: S029HPH
text:
APRILE 2022 is analogous to AN 2020, and their limit was corrected in the erratum to this paper: APRILE 2024B. They set limits chi < 2E-12 (eV/mass(gamma^')) for mass(gamma^') < 3 eV (90% C.L.). For mass(gamma^') > 3 eV, see Fig. 1 of APRILE 2024B.


pdgid: S029HPH
text:
APRILE 2022 extend APRILE 2019 to lower masses by removing the background of ionization signals correlated with high-energy events. The quoted limit applies to mass(gamma^') = 0.09 keV. See their Fig. 15 for mass-dependent limits.


pdgid: S029HPH
text:
APRILE 2022B is an update of APRILE 2020, and set limits chi ~< 5E-17 -- 2E-13. The quoted limit applies to mass(gamma^') = 1 keV. They exclude the XENON1T excess found in APRILE 2020. See their Fig. 6 for mass-dependent limits.


pdgid: S029HPH
text:
BATTAGLIERI 2022 is analogous to BATELL 2014, and derived limits from the electron beam dump experiment at Jefferson Lab (BDX-MINI). Limits at the level of 7E-5 -- 1E-2 are obtained for the dark matter mass mass(gamma^')/3 and the hidden gauge coupling  alpha(D) = 0.1. See their Fig. 11.


pdgid: S029HPH
text:
BOLTON 2022 use the Ly-alpha forest at z ~= 0.1 as a calorimeter for heating in the intergalactic medium by the resonant conversion of hidden photon dark matter to photons, which is assumed to be responsible for the tension between the predicted and observed Ly-alpha absorption linewidths.


pdgid: S029HPH
text:
CERVANTES 2022 use a dielectrically loaded Fabry-Perot open cavity to look for hidden photon dark matter. The local density rho(gamma^') = 0.45 GeV/cm**3 is assumed. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
CHILES 2022 look for hidden photon dark matter by using a layered dielectric target and a superconducting nanowire single-photon detector. The local density rho(gamma^') = 0.4 GeV/cm**3 is assumed. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
HOCHBERG 2022 update HOCHBERG 2019. The quoted limit applies to mass(A0) ~= 11  eV. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
LEES 2022 look for a hidden fermion-fermion bound state decaying into three hidden photons, which subsequently decay into e+ e-, mu+ mu-, or pi+ pi-. For the bound-state mass in the range of 0.05 -- 9.5 GeV, limits at the level of 5E-5 -- 1E-3 are obtained. See their Fig. 6 for mass-dependent limits.


pdgid: S029HPH
text:
LU 2022 derive the limit by studying the effect of photons oscillating into hidden photons on  the surface luminosity of the neutron star RX J1856.6-3754.


pdgid: S029HPH
text:
MANENTI 2022 look for hidden photon dark matter by using a multilayer dielectric haloscope.  Limits between 6.86E-11 and 5E-8 are obtained for mass(gamma^') ~= 1.1 -- 3.1  eV. See their Fig. 11 for mass-dependent limits.


pdgid: S029HPH
text:
THOMAS 2022 improved KRIBS 2021 by taking account of the changes in the parton  distribution functions due to the inclusion of hidden photons. The quoted limit is at mass(gamma^') ~= 4 GeV. Limits in the range of 3E-2 -- 9E-2 are obtained for mass(gamma^') = 1 -- 80 GeV. See their Fig. 1 for the limits.


pdgid: S029HPH
text:
TUMASYAN 2022AH look for exotic decays of the SM-like Higgs boson, H --> Z gamma^' --> 4 lepton, and set limits on the Higgs portal coupling. See their Fig. 6 for the limits.


pdgid: S029HPH
text:
TUMASYAN 2022N look for exotic decays of the SM-like Higgs boson, H --> gamma^' gamma^' (gamma^' --> mu+ mu-), and set limits on the branching fraction product. See their Fig. 7 for mass- and lifetime-dependent limits.


pdgid: S029HPH
text:
WU 2022A look for direction-dependent oscillations in the gravitational potential generated by ultralight hidden photon dark matter, and set a bound on its local density as rho(gamma^') ~< 5 GeV/cm**3 for mass(gamma^') ~< E-23 eV at 95% CL.


pdgid: S029HPH
text:
ANDREEV 2021 is analogous to BANERJEE 2018A. The quoted limit applies to mass(gamma^') = 1 MeV. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
ANDREEV 2021A extends the limits of BANERJEE 2019 by taking account of production through the resonant annihilation of secondary positrons with atomic electrons. The quoted limit is at mass(gamma^') = 0.23 GeV, assuming the fermion dark matter of mass mass(gamma^')/3 and the hidden gauge coupling alpha(D) = 0.1. See their Fig.3 for mass-dependent limits.


pdgid: S029HPH
text:
BI 2021 look for the gamma-ray spectral attenuation due to scattering with hidden photons constituting all dark matter, using the measurements of sub-PeV gamma-rays from the Crab Nebula  by the Tibet ASgamma and HAWC experiments, together with MAGIC and HEGRA gamma-ray  data.  See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
CAZZANIGA 2021 look for semi-visible decays of hidden photons, gamma^' --> chi_1 chi_2 (chi_2 --> chi_1 e+ e-), where chi_{{1}} and chi_{{2}} are hidden fermions. They exclude 3E-5 ~< chi ~< 2E-2 assuming the hidden gauge coupling alpha_{{D}} = 0.1, and the fermion masses mass(chi_{{1}}) = mass(gamma^')/3, (mass(chi_{{2}}) - mass(chi_{{1}}))/mass(chi_{{1}}) = 0.4. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
DIXIT 2021 look for hidden photon dark matter by using a superconducting transmon qubit  dispersively coupled to a high Q storage cavity. The local density  rho(gamma^') = 0.4 GeV/cm**3 is assumed. See their Fig.4 for mass-dependent  limits.


pdgid: S029HPH
text:
GHOSH 2021 use existing haloscope axion search limits to set limits on hidden photon dark matter, considering the polarization of hidden photons. The quoted limit is at mass(gamma^') ~= 3 mueV. See their Fig. 1 for mass-dependent limits.


pdgid: S029HPH
text:
GODFREY 2021 look for hidden photon dark matter by using a wideband antenna, and set 5sigma limits on chi. The local density rho(gamma^') = 0.38  GeV/cm**3 is assumed. See their updated Fig. 12 in arXiv:2101.02805v4 for mass-dependent  limits in the range of mass(gamma^')  = 0.207 -- 1.24 mueV.


pdgid: S029HPH
text:
KOPYLOV 2021A is an update of KOPYLOV 2019, but use Ne gas instead of Ar. The quoted limit applies to mass(gamma^') = 12 eV. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
KRIBS 2021 used the HERA data on neutral current deep inelastic e p scattering to derive the limits, which become weaker for heavier masses. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
SCHMIDT 2021 use the microscopic Parton-Hadron-String Dynamics approach to extract limits by comparing the theoretically calculated dilepton spectra with the HADES data on the search for gamma^' --> e+ e-. See their Fig. 5 for the mass-dependent limits for various allowed surplus of the hidden photon contribution over the standard model yield.


pdgid: S029HPH
text:
TSAI 2021 update the limits from the CHARM and NuCal experiments, taking account of additional production channels from proton bremsstrahlung and eta meson decays, respectively. Limits between 3E-8 and 1E-4 are obtained for 0.01 < mass(gamma^') < 0.8 GeV (see their Fig. 1).


pdgid: S029HPH
text:
AAIJ 2020C look for hidden photons produced from the p p collision in the decay channel gamma^' --> mu+ mu-. For prompt decaying hidden photons, limits at the level of E-4 -- E-3 are obtained for mass(gamma^') = 0.214 -- 30 GeV. See their Fig. 2 for mass-dependent limits.


pdgid: S029HPH
text:
AAIJ 2020C look for hidden photons produced from the p p collision in the decay channel gamma^' --> mu+ mu-. For hidden photons with lifetimes of order ps, limits at the level of E-5 are obtained for mass(gamma^') = 218 -- 315 MeV. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
ABLIKIM 2020AB search for J/psi --> eta^' gamma^' (gamma^' --> gamma pi0), and set the upper limit on the product branching fraction of order E-7. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
AGOSTINI 2020 is analogous to ABE 2014F. The quoted limit applies to mass(gamma^') = 150 keV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. Their limits in their Fig. 3 were later found to be incorrect due to an error of their Eqs. (1) and (2). See Fig. 3 in AGOSTINI 2022A for the corrected limits.


pdgid: S029HPH
text:
AMARAL 2020 use a second-generation SuperCDMS high-voltage eV-resolution detector to set  limits on dark-matter hidden photon absorption. The quoted limit is for mass(gamma^') ~= 17  eV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
AN 2020 updates the direct detection limit of AN 2013C on solar flux of hidden photons;  chi < 1.6E-12 (eV/mass(gamma^')) for mass(gamma^') < 6 eV (90% C.L.). For mass(gamma^') > 6 eV, see their Fig. 1 for mass-dependent limits.


pdgid: S029HPH
text:
ANDRIANAVALOMAHEFA 2020 is analogous to SUZUKI 2015, but uses a mirror that is about one order of magnitude larger than in similar studies in the past. Limits at the level of E-12 are obtained for mass(gamma^') = 2.5 -- 7 eV. See their Fig.23 and Table III for mass-dependent limits.


pdgid: S029HPH
text:
APRILE 2020 is analogous to ABE 2014F, and set limits chi ~< E-16 -- E-12. The quoted limit applies to mass(gamma^') = 1 keV. They also found an excess over known backgrounds, which favors the mass mass(gamma^') = 2.3+-0.2 keV with a 3 sigma significance. See their Fig. 10 for mass-dependent limits.


pdgid: S029HPH
text:
ARALIS 2020 is analogous to ABE 2014F. The quoted limit applies to mass(gamma^') = 0.1 keV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. The limits at masses above 3 keV in their Fig. 10 was later found to be incorrect due to an error in their analysis. See Fig. 3 in erratum for the corrected limits.


pdgid: S029HPH
text:
ARGUELLES 2020 examine hidden-photon production in atmospheric cosmic-ray showers and its decay in IceCube and Super-Kamiokande. The quoted limit assumes a lifetime of ctau = 0.1 km. See their Fig. 16 for mass- and lifetime-dependent limits.


pdgid: S029HPH
text:
ARNAUD 2020 look for the absorption signal of hidden photon dark matter in a Ge detector. The quoted limit applies to mass(gamma^') ~= 9 eV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
BANERJEE 2020 is an update of BANERJEE 2018. They exclude 8.2E-5 ~< chi ~< 1E-2 for mass(gamma^') = 1.5 -- 24 MeV. In particular, they exclude chi = 1.2E-4 -- 6.8E-4 for the 16.7 MeV gauge boson. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
BARAK 2020 is analogous to AGUILAR-AREVALO 2019A, and look for hidden photon dark matter by using the Skipper CCD. The quoted limit applies to mass(gamma^') = 12.8 eV. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
KRASNIKOV 2020 showed that the limit of BANERJEE 2020 combined with the measured anomalous magnetic moment of the electron exclude the 16.7 MeV gauge boson suggested by the ATOMKI (KRASZNAHORKAY 2016) experiment if it has pure vector or axial-vector interactions.


pdgid: S029HPH
text:
SHE 2020 look for solar hidden photons. The quoted limit applies to mass(gamma^') = 180 eV. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
SHE 2020 look for hidden photon dark matter and set limits chi < 1.3E-15 -- 2.8E-14 for the quoted mass range. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed.  See their Fig. 6 for mass-dependent limits.


pdgid: S029HPH
text:
SIRUNYAN 2020AQ look for a narrow resonance decaying into a pair of muons. For mass(gamma^') < 45 GeV, they use dedicated high-rate dimuon triggers to reduce the muon transverse momentum thresholds. The quoted limit applies to mass(gamma^') = 50 GeV, and limits of order E-3 are obtained for the quoted mass range. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
TOMITA 2020 look for hidden photon dark matter using a planar metal plate and cryogenic receiver and set limits chi < 1.8 -- 4.3E-10 for the quoted mass range. The local density rho(gamma^') = 0.39 GeV/cm**3 is assumed. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
WANG 2020A is analogous to ABE 2014F. The quoted limit applies to mass(gamma^') = 185 eV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 11 for mass-dependent limits.


pdgid: S029HPH
text:
AABOUD 2019G look for h --> gamma^' gamma^' (gamma^' --> mu+ mu-) and exclude a kinetic mixing around E-9 -- E-8 for B(h --> gamma^' gamma^') = 0.01 and 0.1. See their Fig. 9 for mass-dependent limits.


pdgid: S029HPH
text:
ABLIKIM 2019A look for J/psi --> gamma^' eta (gamma^' --> e+ e-). Limits between 6E-3 and 5E-2 are obtained (see their Fig. 8).


pdgid: S029HPH
text:
ABLIKIM 2019H look for J/psi --> gamma^' eta^' (gamma^' --> e+ e-). Limits between 3.4E-3 and 2.6E-2 are obtained. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
AGUILAR-AREVALO 2019A look for the absorption signal of hidden photon dark matter by using a CCD. The quoted limit applies to mass(gamma^') = 17 eV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
APRILE 2019D is analogous to ABE 2014F. The quoted limit applies to mass(gamma^') = 0.7 keV. See their Fig. 5(f) for mass-dependent limits.


pdgid: S029HPH
text:
BANERJEE 2019 is an update of BANERJEE 2018A. The quoted limit is at mass(gamma^') = 1 MeV. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
BHOONAH 2019 examine heating of Galactic Center gas clouds by hidden photon dark matter. The quoted limit applies to mass(gamma^') ~= E-12 eV. See their Fig. 2 for mass-dependent limits.


pdgid: S029HPH
text:
BRUN 2019 is analogous to SUZUKI 2015. The limit is derived under an assumption that hidden photons constitute the local dark matter density rho(gamma') = 0.3 GeV/cm**3.


pdgid: S029HPH
text:
CORTINA-GIL 2019 look for an invisible hidden photon in the reaction K+ --> pi+ pi0 (pi0 --> gamma gamma^'). The quoted limit applies to mass(gamma^') = 62.5 -- 65 MeV. See their Figs. 6 and 7 for mass-dependent limits.


pdgid: S029HPH
text:
DANILOV 2019 examined the hidden photon production in nuclear reactors, correctly taking account of the effective photon mass in the reactor and detector. The limit gets weaker for mass(gamma^') less than the effective photon mass in proportion to 1/mass**2(gamma^'). See their Fig. 1 for mass-dependent limits.


pdgid: S029HPH
text:
HOCHBERG 2019 look for the absorption signal of hidden photon dark matter by using superconducting-nanowire single-photon detectors. The quoted limit applies to mass(gamma^') ~= 1 eV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
KOPYLOV 2019 look for hidden-photon dark matter using a counter with an aluminum cathode and derive limits assuming it constitute all the local dark matter. The quoted limit applies to mass(gamma^') = 12 eV. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
KOVETZ 2019 examine heating of the early Universe plasma by hidden photon dark matter, and derive the limits by requiring that the cosmic mean 21 cm brightness temperature relative to the CMB temperature satisfy T(21) > -100 mK. The quoted limit applies to mass(gamma^') ~= 2E-14 eV. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
NGUYEN 2019 look for hidden photon dark matter with a resonant cavity, and set limits ~E-12 for mass(gamma^') = 0.2 -- 2.07mueV. The quoted limit applies to mass(gamma^') = 1.3 mueV. The local density rho(gamma^') = 0.3 GeV/cm**3 is assumed. See their Fig. 19 for mass-dependent limits.


pdgid: S029HPH
text:
ABE 2018F is an update of ABE 2014F. The quoted limit applies to mass(gamma^') ~= 40 keV. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
ADRIAN 2018 look for a hidden photon resonance in the reaction e- Z --> e- Z gamma^' (gamma^' --> e+ e-). The quoted limit applies to mass(gamma^') = 40 MeV. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
ANASTASI 2018B look for a hidden photon resonance in the reaction e+ e- --> gamma^' gamma (gamma^' --> mu+ mu-). The quoted limit is obtained by combining the result of ANASTASI 2016 and it applies to mass(gamma^') ~= 519 -- 987 MeV. See their Fig. 9 for mass-dependent limits.


pdgid: S029HPH
text:
ARMENGAUD 2018 is analogous to ABE 2014F. The quoted limits applies to mass(gamma^') = 1.6 keV. See the right panel of Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
BANERJEE 2018 look for hidden photons produced in the reaction e- Z --> e- Z gamma^' (gamma^' --> e+ e-), and exclude 9.2E-5 ~< chi ~< 1E-2 for mass(gamma^') = 1 -- 23 MeV. They also set a limit on the electron coupling to a 16.7 MeV gauge boson suggested by the ATOMKI (KRASZNAHORKAY 2016) experiment. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
BANERJEE 2018A look for invisible decays of hidden photons produced in the reaction e- Z --> e- Z gamma^'. The quoted limit is at mass(gamma^') = 1 MeV. See their Fig. 15 for mass-dependent limits.


pdgid: S029HPH
text:
ABGRALL 2017 is analogous to ABE 2014F using the MAJORANA DEMONSTRATOR. See their Fig. 3 for limits between 6 keV < mass(gamma^') < 97 keV.


pdgid: S029HPH
text:
ABLIKIM 2017AA look for e+ e- --> gamma gamma^' (gamma^' --> e+ e- or mu+ mu-). Limits between E-3 and E-4 are obtained (see their Fig. 3).


pdgid: S029HPH
text:
ANGLOHER 2017 is analogous to ABE 2014F. The quoted limit is at mass(gamma^') = 0.7 keV. See their Fig. 8 for mass-dependent limits.


pdgid: S029HPH
text:
BANERJEE 2017 look for invisible decays of hidden photons produced in the reaction e- Z --> e- Z gamma^'. The quoted limit applies to mass(gamma^') = 2 MeV. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
CHANG 2017 examine the hidden photon emission from SN1987A, including the effects of finite temperature and density on chi and obtain limits chi (mass(gamma^')/MeV) ~< 3E-9 for mass(gamma^') < 15 MeV and chi ~< E-9 for mass(gamma^') = 15 -- 120 MeV.


pdgid: S029HPH
text:
DUBININA 2017 look for mu+ --> e+ nubar_mu nu_e gamma^' (gamma^' --> e+ e-) in a nuclear photoemulsion. The quoted limit applies to mass(gamma^') = 1.1 MeV. Limits between 4.5E-3 and E-2 are obtained (see their Fig. 3).


pdgid: S029HPH
text:
LEES 2017E look for invisible decays of hidden photons produced in the reaction e+ e- --> gamma gamma^'. See their Fig. 5 for limits in the mass range mass(gamma^') <= 8 GeV.


pdgid: S029HPH
text:
AAD 2016AG look for hidden photons promptly decaying into collimated electrons and/or muons, assuming that they are produced in the cascade decays of squarks or the Higgs boson. See their Fig. 10 and Fig.13 for their limits on the cross section times branching fractions.


pdgid: S029HPH
text:
ANASTASI 2016 look for the decay gamma^' --> pi+ pi- in the reaction e+ e- --> gamma gamma^'. Limits between 4.3E-3 and 4.4E-4 are obtained for 527 < mass(gamma^') < 987 MeV (see their Fig. 9).


pdgid: S029HPH
text:
KHACHATRYAN 2016 look for gamma^' --> mu+ mu- in a dark SUSY scenario where the SM-like Higgs boson decays into a pair of the visible lightest neutralinos with mass 10 GeV, both of which decay into gamma^' and a hidden neutralino with mass 1 GeV. See the right panel in their Fig. 2.


pdgid: S029HPH
text:
AAD 2015CD look for H --> Z gamma^' --> 4 lepton with the ATLAS detector at LHC and find chi < 4 -- 17E-2 for mass(gamma^') = 15 -- 55 GeV. See their Fig. 6.


pdgid: S029HPH
text:
ADARE 2015 look for a hidden photon in pi0, eta0 --> gamma e+ e- at the PHENIX experiment. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
AN 2015A derived limits from the absence of ionization signals in the XENON10 and XENON100  experiments, assuming hidden photons constitute all the local dark matter. Their best limit is chi < 1.3E-15 at mass(gamma^') = 18 eV. See their Fig. 1 for mass-dependent  limits.


pdgid: S029HPH
text:
ANASTASI 2015 look for a production of a hidden photon and a hidden Higgs boson with the KLOE detector at DAPhiNE, where the hidden photon decays into a pair of muons and the hidden Higgs boson lighter than mass(gamma^') escape detection. See their Figs. 6 and 7 for mass-dependent limits on a product of the hidden fine structure constant and the kinetic mixing.


pdgid: S029HPH
text:
ANASTASI 2015A look for the decay gamma^' --> e+ e- in the reaction e+ e- --> e+ e- gamma. Limits between 1.7E-3 and 1E-2 are obtained for mass(gamma^') = 5 -- 320 MeV (see their Fig. 7).


pdgid: S029HPH
text:
BATLEY 2015A look for pi0 --> gamma gamma^' (gamma^' --> e+ e-) at the NA48/2 experiment. Limits between 4.2E-4 and 8.8E-3 are obtained for mass(gamma^') = 9 -- 120 MeV (see their Fig. 4).


pdgid: S029HPH
text:
JAEGLE 2015 look for the decay gamma^' --> e+ e-, mu+ mu-, or pi+ pi- in the dark Higgstrahlung channel, e+ e- --> gamma^' H^' (H^' --> gamma^' gamma^') at the BELLE experiment. They set limits on a product of the branching fraction and the Born cross section as well as a product of the hidden fine structure constant and the kinetic mixing. See their Figs. 3 and 4.


pdgid: S029HPH
text:
KAZANAS 2015 set limits by studying the decay of hidden photons gamma^' --> e+ e- inside and near the progenitor star of SN1987A. See their Fig. 6 for mass-dependent limits.


pdgid: S029HPH
text:
SUZUKI 2015 looked for hidden-photon dark matter with a dish antenna and derived limits assuming they constitute all the local dark matter. Their limits are chi < 6E-12 for mass(gamma^') = 1.9 -- 4.3 eV. See their Fig. 7 for mass-dependent limits.


pdgid: S029HPH
text:
VINYOLES 2015 performed a global fit analysis based on helioseismology and solar neutrino observations, and set the limits chimass(gamma^') < 1.8E-12 eV for mass(gamma^') = 3E-5 -- 8 eV. See their Fig. 11.


pdgid: S029HPH
text:
ABE 2014F look for the photoelectric-like interaction in the XMASS detector assuming the hidden photon constitutes all the local dark matter. Limits between 2E-13 and 1E-12 are obtained, where the relation chi**2 = alpha'/alpha is used to translate the original bound on the ratio of the hidden and EM fine-structure constants. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
AGAKISHIEV 2014 look for hidden photons gamma^' --> e+ e- at the HADES experiment, and set limits on chi for mass(gamma^') = 0.02 -- 0.6 GeV. See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
BABUSCI 2014 look for the decay gamma^' --> mu+ mu- in the reaction e+ e- --> mu+ mu- gamma. Limits between 4E-3 and 9.0E-4 are obtained for 520 MeV < mass(gamma^')< 980 MeV (see their Fig. 7).


pdgid: S029HPH
text:
BATELL 2014 derived limits from the electron beam dump experiment at SLAC (E-137) by searching for events with recoil electrons by sub-GeV dark matter produced from the decay of the hidden photon. Limits at the level of E-4 -- E-1 are obtained for mass(gamma^') = E-3 -- 1 GeV, depending on the dark matter mass and the hidden gauge coupling (see their Fig. 2).


pdgid: S029HPH
text:
BLUEMLEIN 2014 analyzed the beam dump data taken at the U-70 accelerator to look for gamma^'-bremsstrahlung and the subsequent decay into muon pairs and hadrons. See their Fig. 4 for mass-dependent excluded region.


pdgid: S029HPH
text:
FRADETTE 2014 studied effects of decay of relic hidden photons on BBN and CMB to set constraints on very small values of the kinetic mixing. See their Figs. 4 and 7 for mass-dependent excluded regions.


pdgid: S029HPH
text:
LEES 2014J look for hidden photons in the reaction e+ e- --> gamma gamma^' (gamma^' --> e+ e-, mu+ mu-). Limits at the level of E-4 -- E-3 are obtained for 0.02 GeV < mass(gamma^') < 10.2 GeV. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
MERKEL 2014 look for gamma^' --> e+ e- at the A1 experiment at the Mainz Microtron (MAMI). See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
AN 2013B examined the stellar production of hidden photons, correcting an important error of the production rate of the longitudinal mode which now dominates. See their Fig. 2 for mass-dependent limits based on solar energy loss.


pdgid: S029HPH
text:
AN 2013C use the solar flux of hidden photons to set a limit on the atomic ionization rate in the XENON10 experiment. They find chi mass(gamma^') < 3E-12 eV for  mass(gamma^')< 1 eV. See their Fig. 2 for mass-dependent limits.


pdgid: S029HPH
text:
DIAMOND 2013 analyzed the beam dump data taken at the SLAC millicharge experiment to constrain a hidden photon invisibly decaying into lighter long-lived particles, which undergo elastic scattering off nuclei in the detector. Limits between 8E-4 -- 2E-2 are obtained. The quoted limit is applied when the dark gauge coupling is set equal to the electromagnetic coupling. See their Fig.4 for mass-dependent limits.


pdgid: S029HPH
text:
GNINENKO 2013 used the data taken at the SINDRUM experiment to constrain the decay, pi0 --> gamma gamma^' (gamma^' --> e+ e-) to derive limits. See their Fig. 2 for their mass-dependent excluded region.


pdgid: S029HPH
text:
HORVAT 2013 look for hidden-photo-electric effect in HPGe detectors induced by solar hidden photons. See their Fig. 3 for mass-dependent limits.


pdgid: S029HPH
text:
INADA 2013 search for hidden photons using an intense X-ray beamline at SPring-8. See their Fig. 4 for mass-dependent limits.


pdgid: S029HPH
text:
PARKER 2013 look for hidden photons using a cryogenic resonant microwave cavity. See their Fig.5 for mass-dependent limits.


pdgid: S029HPH
text:
REDONDO 2013 examined the solar emission of hidden photons including the enhancement factor for the longitudinal mode pointed out by AN 2013B, and also updated stellar-energy loss arguments. See their Fig.3 for mass-dependent limits, including a review of the currently best limits from other arguments.


pdgid: S029HPH
text:
GNINENKO 2012A obtained bounds on B(pi0 --> gamma gamma^'). B(gamma^' --> e+ e-) from the NOMAD and PS191 neutrino experiments, and derived limits between 8E-8 -- 2E-4. See their Fig.4 for mass-dependent excluded regions.


pdgid: S029HPH
text:
GNINENKO 2012B used the data taken at the CHARM experiment to constrain the decay, eta(eta^') gamma gamma^' (gamma^' --> e+ e-), and derived limits between 1E-7 -- 1E-4. See their Fig.4 for mass-dependent excluded region.


pdgid: S029HPH
text:
ABRAHAMYAN 2011 look for gamma^' --> e+ e- in the electron-nucelon fixed-target experiment at the Jefferson Laboratory (APEX). See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
BLUEMLEIN 2011 analyzed the beam dump data taken at the U-70 accelerator to look for pi0 --> gamma gamma^' (gamma^' --> e+ e-). See their Fig. 5 for mass-dependent limits.


pdgid: S029HPH
text:
BJORKEN 2009 analyzed the beam dump data taken at E137, E141, and E774 to constrain a hidden photon produced by bremsstrahlung, subsequently decaying into e+ e-, and derived limits between E-7 and E-2. See their Fig. 1 for mass-dependent excluded region.


pdgid: S029HPH
text:
BJORKEN 2009 required the energy loss in the gamma^' emission from the core of SN1987A not to exceed E53 erg/s, and derived limits between 5E-9 and 2E-6. See their Fig. 1 for mass-dependent excluded region.


pdgid: S003AMU
text:
BEIER 2002 compares Larmor frequency of the electron bound in a C12**5+ ion with the cyclotron frequency of a single trapped C12**5+ ion.


pdgid: S003AMU
text:
FARNHAM 1995 compares cyclotron frequency of trapped electrons with that of a single trapped C12**6+ ion.


pdgid: S003M
text:
Converted to MeV using the 1998 CODATA value of the conversion constant, 931.494013+-0.000037 MeV/u.


pdgid: S003DM
text:
FEE 1993 value is obtained under the assumption that the positronium Rydberg constant is exactly half the hydrogen one.


pdgid: S003DM
text:
DOLGOV 2014 result is obtained under the assumption that any mass difference between electron and positron would lead to a non-zero photon mass. The PDG 2012 limit of 1E-18 eV on the photon mass is in turn used to derive the value quoted here.


pdgid: S003DQ
text:
MUELLER 1992 argues that an inequality of the charge magnitudes would, through higher-order vacuum polarization, contribute to the net charge of atoms.


pdgid: S003MM
text:
FAN 2023 report the most accurate measurement of the electron magnetic moment. A one-electron  quantum cyclotron is used. We do not propagate at the moment this measurement to the fine structure and other physical constants. When discrepancies in the independent determinations of alpha are resolved, the new measurement uncertainty of 0.13 ppt is available for precise tests for BSM physics.


pdgid: S003MM
text:
This VANDYCK 1987 reault is for a positron. We do not take it into account for the average to avoid the assumption of CPT invariance.


pdgid: S003EDM
text:
ABDULLAH 1990, COMMINS 1994, and REGAN 2002 use the relativistic enhancement of a valence electron's electric dipole moment in a high-Z atom.


pdgid: S003T
text:
AGOSTINI 2024A search for coincident photons from the direct e-decay and from residual X-ray or Auger-e transitions.


pdgid: S003T
text:
The authors of A. Derbin et al, arXiv:0704.2047v1 argue that this limit is overestimated by at least a factor of 5.


pdgid: S003T
text:
ORITO 1985 assumes that electromagnetic forces extend out to large enough distances and that the age of our galaxy is 10**10 years.


pdgid: S003TD
text:
ARNQUIST 2024B limit on charge nonconserving e- capture in 37.5 kg high-purity Ge implies limit on e --> nu nubar nu or more generally e --> invisible.


pdgid: S003TD
text:
BELLI 1999B limit on charge nonconserving e- capture involving excitation of the 236.1 keV nuclear state of Xe129. The 90% CL limit is >3.7 yr. Less stringent limits for other states are also given.


pdgid: S003TD
text:
BELLI 1999D limit on charge nonconserving e- capture involving excitation of the 57.6 keV nuclear state of I127. Less stringent limits for the other states and for the state of Na23 are also given.


pdgid: S004MM
text:
AGUILLARD 2025 quote the combined value from all RUNS 1 -- 6 (at 127 ppm precision). For the 2020 -- 2023 data (Runs 4, 5, 6) alone AGUILLARD 2025 measure a value of 11659207.10+-1.62E-10 (at precision of 139 ppb).


pdgid: S004MM
text:
This AGUILLARD 2023 value is the combination of all 2018, 2019 and 2020 data, including the ABI 2021 value. The new FNAL 2019 and 2020 data alone combined yield 11659205.7+-2.5E-10.


pdgid: S004MM
text:
ABI 2021 combined their value with the previous independent BNL measurement of BENNETT 2006. ABI 2021 also report that the difference of this combination with the standard model value of 11659181.0+-4.3E-10 (AOYAMA 2020) has a significance of 4.2 sigma.


pdgid: S004MM
text:
BAILEY 1979 values recalculated by HUGHES 1999 using the COHEN 1987 mu/p magnetic moment. The improved MOHR 1999 value does not change the result.


pdgid: S004EDM
text:
This is the combination of the two BENNETT 2009 measurements quoted here separately for mu+ and mu-. The result is also presented as a measurement of 0.0+-0.9E-19e cm.


pdgid: S004EDM
text:
EMA 2022 determine indirect constraints on |mu_{{EDM}}| from EDM measurements performed on heavy atoms and molecules, based on the muon-loop induced light-by-light CP-odd amplitude.


pdgid: S004EDM
text:
This is the combination of the two BAILEY 1978 results quoted here separately for mu+ and mu-. BAILEY 1978 uses the convention d = 1/2. (d(mu+)- d(mu-)) and reports 3.7+-3.4. We convert their result to use the same convention as BENNETT 2009.


pdgid: S004MEC
text:
MEYER 2000 measure the 1s-2s muonium interval, and then interpret the result in terms of muon-electron charge ratio q(mu+)/q(e-).


pdgid: S004R1
text:
BALDINI 2016 measurement refers to mu+ --> e+ nu nubar gamma decay and requires energy of e+> 45 MeV and energy gamma > 40 MeV.


pdgid: S004R6
text:
CRITTENDEN 1961 count only those decays where total energy of either (e+, e-) combination is >10 MeV.


pdgid: S004R6
text:
GUREVICH 1960 interpret their event as either virtual or real photon conversion. e+ and e- energies not measured.


pdgid: S004R6
text:
In the three LEE 1959 events, the sum of energies E(e+) + E(e-) + E(e+) was 51 MeV, 55 MeV, and 33 MeV.


pdgid: S004R2
text:
FREEDMAN 1993 limit on nubar_{{e}} observation is here interpreted as a limit on lepton family number violation.


pdgid: S004R2
text:
BERGSMA 1983 gives a limit on the inverse muon decay cross-section ratio CS(nubar_mu e- --> mu- nubar_e)/CS(nu_mu e- --> mu- nu_e), which is essentially equivalent to G(mu- --> e- nu_e nubar_mu)/G(total) for small values like that quoted.


pdgid: S004R3
text:
AFANACIEV 2025A is based on all 2021-2022 data and supersedes previous results. A combination of MEG/MEG II would only improve the limit by a few % and thus is not reported separately by AFANACIEV 2025A.


pdgid: S004R3
text:
AFANACIEV 2024 reports results using data collected by MEGII in 2021 combined with the limit obtained by the MEG experiment. Supersedes BALDINI 2016.


pdgid: S004R5
text:
BALDINI 2020 uses 7.5E14 stopped muons to obtain limits on mu --> e X decay mediated by a new light particle X with lifetimes < 40 ps, which decays to gamma gamma for X-mass ranges 20 -- 45 MeV. The limit of the order < E-11 at 90% CL is for the mass range 20 -- 30 MeV.


pdgid: S004RG
text:
DOHMEN 1993 assumes mu- --> e- conversion leaves the nucleus in its ground state, a process enhanced by coherence and expected to dominate.


pdgid: S004RP2
text:
ABELA 1980 is upper limit for mu- e+ conversion leading to particle-stable states of Sb127. Limit for total conversion rate is higher by a factor less than 4 (G. Backenstoss, private communication).


pdgid: S004RP4
text:
This limit assumes a giant resonance excitation of the daughter Ca nucleus (mean energy and width both 20 MeV).


pdgid: S004RP4
text:
This limit assumes the daughter Ca nucleus is left in the ground state. However, the probability of this is unknown.


pdgid: S004MC
text:
WILLMANN 1999 quote both probability P(M Mbar)<8.3E-11 at 90%CL in a 0.1 T field and R(g)= G(C)/G(F).


pdgid: S004RHO
text:
The quoted systematic error includes a contribution of 0.00013 (added in quadrature) from uncertainties on radiative corrections and on the Michel parameter eta.


pdgid: S004RHO
text:
The quoted systematic error includes a contribution of 0.00011 (added in quadrature) from the dependence on the Michel parameter eta.


pdgid: S004RHO
text:
The quoted systematic error includes a contribution of 0.00023 (added in quadrature) from the dependence on the Michel parameter eta.


pdgid: S004RHO
text:
eta constrained = 0. These values incorporated into a two parameter fit to rho and eta by DERENZO 1969.


pdgid: S004ETA
text:
Previously we used the global fit result from BURKARD 1985B in OUR AVERAGE, we now only include their actual measurement.


pdgid: S004DEL
text:
The quoted systematic error includes a contribution of 0.00006 (added in quadrature) from uncertainties on radiative corrections and on the Michel parameter eta.


pdgid: S004DEL
text:
VOSSLER 1969 has measured the asymmetry below 10 MeV. See comments about radiative corrections in VOSSLER 1969.


pdgid: S004XI
text:
The corresponding 90% confidence limit from IMAZATO 1992 is |xiP_{{mu}}| >0.990. This measurement is of K+ decay, not pi+ decay, so we do not include it in an average, nor do we yet set up a separate data block for K results.


pdgid: S004XID
text:
BAYES 2011 obtains the limit > 0.99909 (90% CL) with the constraint that xi*(mu LONGITUDINAL POLARIZATION)*delta/rho <= 1.0.


pdgid: S004XID
text:
STOKER 1985 find (xi*P(mu)*delta/rho) >0.9955 and >0.9966, where the first limit is from new mu spin-rotation data and the second is from combination with CARR 1983 data. In V-A theory, (delta/rho) = 1.0.


pdgid: S004ALP
text:
Previously we used the global fit result from BURKARD 1985B in OUR AVERAGE, we now only include their actual measurement. BURKARD 1985B measure e+ polarizations P(T(1)) and P(T(2)) versus e+ energy.


pdgid: S035M
text:
ADACHI 2023C, AUBERT 2009AK and BELOUS 2007 fit tau pseudomass spectrum in tau --> pi pi+ pi- nu_tau decays. Result assumes mass(nu_{{tau}}) = 0.


pdgid: S035M
text:
ABBIENDI 2000A fit tau pseudomass spectrum in tau --> pi+- <=2pi0 nu_tau and tau --> pi+- pi+ pi- <=1pi0 nu_tau decays. Result assumes mass(nu_{{tau}})=0.


pdgid: S035M
text:
ALBRECHT 1992M fit tau pseudomass spectrum in tau- --> 2pi- pi+ nu_tau decays. Result assumes mass(nu_{{tau}})=0.


pdgid: S035M
text:
BACINO 1978B value comes from e+- X-+ threshold. Published mass 1782 MeV increased by 1 MeV using the high precision psi(2S) mass measurement of ZHOLENTZ 1980 to eliminate the absolute SPEAR energy calibration uncertainty.


pdgid: S035M
text:
BALEST 1993 fit spectra of minimum kinematically allowed tau mass in events of the type e+ e- --> tau+ tau- --> (pi+ n pi0 nu_tau)(pi- m pi0 nu_tau) n<=2, m<=2, 1<=n+m<=3. If mass(nu_{{tau}})not=0, result increases by (mass**2(nu_{{tau}})/1100 MeV).


pdgid: S035MDF
text:
AUBERT 2009AK quote both the listed upper limit and (mass(tau+)-mass(tau-))/m(average) = -3.4+-1.3+-0.3E-4.


pdgid: S035MM
text:
AAD 2025BB limits are obtained by comparing the inclusive tau+ tau- fiducial cross-section in p p collisions as a function of visible invariant mass at large masses to the Standard Model prediction.


pdgid: S035MM
text:
Measurement ill-suited for a standard average because its likelihood appears to be remarkably non-Gaussian and asymmetric according to the model-dependent extraction procedure and the reported 95% CL limits.


pdgid: S035MM
text:
AAD 2023BM measurement is derived from gamma gamma --> tau+ tau- total cross-section TeV. Authors report both the measured value and the corresponding 95% CL limit. from 1.44 nb**-1 LHC Pb-Pb collisions at sqrt(S_{{NN}}) = 5.02


pdgid: S035MM
text:
TUMASYAN 2023AS measurement is derived from gamma gamma --> tau+ tau- total cross-section from 404 mub**-1 LHC Pb-Pb collisions at sqrt(S_{{NN}}) = 5.02 TeV.


pdgid: S035MM
text:
ABDALLAH 2004K measurement is derived from e+ e- --> e+ e- tau+ tau- total cross-section measurements at sqrt(s) between 183 and 208 GeV. In addition to the measurement, the authors also quote 95% CL limits of > -0.052 and < 0.013.


pdgid: S035MM
text:
ACHARD 2004G limit is derived from e+ e- --> e+ e- tau+ tau- total cross-section measurements at sqrt(s) between 189 and 206 GeV, and is on the absolute value of the magnetic moment anomaly.


pdgid: S035MM
text:
GONZALEZ-SPRINBERG 2000 use data on tau lepton production at LEP1, SLC, and LEP2, and data from colliders and LEP2 to determine limits. Assume imaginary component is zero.


pdgid: S035MM
text:
ACCIARRI 1998E use Z --> tau+ tau- gamma events. In addition to the limits, the authors also quote a value of 0.004+-0.027+-0.023.


pdgid: S035MM
text:
ACKERSTAFF 1998N use Z --> tau+ tau- gamma events. The limit applies to an average of the form factor for off-shell tau's having p**2 ranging from mass**2(tau) to (M(Z)-mass(tau))**2.


pdgid: S035MM
text:
ESCRIBANO 1993 limit derived from Gamma(Z --> tau+ tau-), and is on the absolute value of the magnetic moment anomaly.


pdgid: S035MM
text:
SILVERMAN 1983 limit is derived from e+ e- --> tau+ tau- total cross-section measurements for q**2 up to (37 GeV)**2.


pdgid: S035EDM
text:
INAMI 2022 use e+ e- --> tau+ tau- events from 833 fb**-1 of data. Also report a measurement of Re(d(tau)) = -0.62+-0.63E-17 ecm.


pdgid: S035EDM
text:
GROZIN 2009A calculate the contribution to the electron electric dipole moment from the tau electric dipole moment appearing in loops, which is Deltad(e) = 6.9E-12 d(tau). Dividing the REGAN 2002 upper limit |d(e)|<=1.6E-27 e cm at CL=90% by 6.9E-12 gives this limit.


pdgid: S035EDM
text:
ABDALLAH 2004K limit is derived from e+ e- --> e+ e- tau+ tau- total cross-section measurements at sqrt(s) between 183 and 208 GeV and is on the absolute value of d_{{tau}}.


pdgid: S035EDM
text:
ACHARD 2004G limit is derived from e+ e- --> e+ e- tau+ tau- total cross-section measurements at sqrt(s) between 189 and 206 GeV, and is on the absolute value of d_{{tau}}.


pdgid: S035EDM
text:
ESCRIBANO 1997 derive the relationship |d(tau)| = cot theta(W)|d(tau)**W| using effective Lagrangian methods, and use a conference result |d(tau)**W| <5.8E-18 e cm at 95% CL (L. Silvestris, ICHEP96) to obtain this result.


pdgid: S035EDM
text:
ESCRIBANO 1993 limit derived from Gamma(Z --> tau+ tau-), and is on the absolute value of the electric dipole moment.


pdgid: S035EDI
text:
INAMI 2022 use e+ e- --> tau+ tau- events from 833 fb**-1 of data. Also report a measurement of Im(d(tau)) = -0.40+-0.32E-17 ecm.


pdgid: S035WDM
text:
Limit is on the absolute value of the real part of the weak dipole moment, and applies for q**2 = mass**2(Z).


pdgid: S035WDI
text:
Limit is on the absolute value of the imaginary part of the weak dipole moment, and applies for q**2 = mass**2(Z).


pdgid: S035B75
text:
The correlation coefficients between this measurement and the ABREU 2001M measurements of B(tau --> 3-prong) and B(tau --> 5-prong) are -0.98 and -0.08 respectively.


pdgid: S035B75
text:
The correlation coefficients between this measurement and the ACHARD 2001D measurements of B(tau --> ``3-prong'') and B(tau --> ``5-prong'') are -0.978 and -0.082 respectively.


pdgid: S035R24
text:
Not independent of ADEVA 1991F G(tau- --> h- h- h+ hboxbgroup>=0 neutrals >=0K0L nu_tau egroup)/G(total) value.


pdgid: S035R24
text:
Not independent of AIHARA 1987B G(tau- --> mu- nubar_mu nu_tau)/G(total), [G(tau- --> e- nubar_e nu_tau)/G(total), and [G(tau- --> h- >=0 neutrals >=0K0L nu_tau)/G(total) values.


pdgid: S035R24
text:
Not independent of SCHMIDKE 1986 value (also not independent of BURCHAT 1987 value for G(tau- --> h- h- h+ hboxbgroup>=0 neutrals >=0K0L nu_tau egroup)/G(total).


pdgid: S035R24
text:
Not independent of ALTHOFF 1985 G(tau- --> mu- nubar_mu nu_tau)/G(total), [G(tau- --> e- nubar_e nu_tau)/G(total), [G(tau- --> h- >=0 neutrals >=0K0L nu_tau)/G(total), and [G(tau- --> h- h- h+ hboxbgroup>=0 neutrals >=0K0L nu_tau egroup)/G(total) values.


pdgid: S035R1
text:
See footnote to SCHAEL 2005C Gamma(tau- --> e- nubar_e nu_tau)/Gamma(total) measurement for correlations with other measurements.


pdgid: S035R1
text:
The correlation coefficient between this measurement and the ACCIARRI 2001F measurement of B(tau- --> e- nubar_e nu_tau) is 0.08.


pdgid: S035R1
text:
The correlation coefficients between this measurement and the ANASTASSOV 1997 measurements of B(e nubar_e nu_tau), B(mu nubar_mu nu_tau)/B(e nubar_e nu_tau), B(h- nu_tau), and B(h- nu_tau)/B(e nubar_e nu_tau) are 0.50, 0.58, 0.50, and 0.08 respectively.


pdgid: S035R1
text:
Not independent of ALBRECHT 1992D Gamma(mu- nubar_mu nu_tau)/Gamma(e- nubar_e nu_tau) and ALBRECHT 1993G Gamma(mu- nubar_mu nu_tau)xGamma(e- nubar_e nu_tau)/Gamma(total)**2 values.


pdgid: S035B81
text:
SHIMIZU 2018A impose requirements on detected gamma's corresponding to a tau-rest-frame energy cutoff E(gamma*) > 10 MeV.


pdgid: S035B81
text:
LEES 2015G impose requirements on detected gamma's corresponding to a tau-rest-frame  energy cutoff E(gamma*) > 10 MeV.


pdgid: S035B81
text:
BERGFELD 2000 impose requirements on detected gamma's corresponding to a tau-rest-frame energy cutoff E(gamma*)>10 MeV. For E(gamma*)>20 MeV, they quote 3.04+-0.14+-0.30E-3.


pdgid: S035B81
text:
ALEXANDER 1996S impose requirements on detected gamma's corresponding to a tau-rest-frame energy cutoff E(gamma)>20 MeV.


pdgid: S035B81
text:
WU 1990 reports Gamma(mu- nubar_mu nu_tau gamma)/Gamma(mu- nubar_mu nu_tau) = 0.013+-0.006, which is converted to Gamma(mu- nubar_mu nu_tau gamma)/Gamma(total) using Gamma(mu- nubar_mu nu_tau gamma)/Gamma(total) = 17.35%. Requirements on detected gamma's correspond to a tau rest frame energy cutoff E_{{gamma}} > 37 MeV.


pdgid: S035R2
text:
The correlation coefficient between this measurement and the ACCIARRI 2001F measurement of B(tau- --> mu- nubar_mu nu_tau) is 0.08.


pdgid: S035R2
text:
The correlation coefficients between this measurement and the ANASTASSOV 1997 measurements of B(mu nubar_mu nu_tau), B(mu nubar_mu nu_tau)/B(e nubar_e nu_tau), B(h- nu_tau), and B(h- nu_tau)/B(e nubar_e nu_tau) are 0.50, -0.42, 0.48, and -0.39 respectively.


pdgid: S035R5
text:
The correlation coefficients between this measurement and the ANASTASSOV 1997 measurements of B(mu nubar_mu nu_tau), B(e nubar_e nu_tau), B(h- nu_tau), and B(h- nu_tau)/B(e nubar_e nu_tau) are 0.58, -0.42, 0.07, and 0.45 respectively.


pdgid: S035C39
text:
BERGFELD 2000 impose requirements on detected gamma's corresponding to a tau-rest-frame energy cutoff E(gamma*)>10 MeV.


pdgid: S035R43
text:
FORD 1987 result for B(pi- nu_tau) with 0.67% added to remove their K- correction and adjusted for 1992 B(``1 prong'').


pdgid: S035R43
text:
BUSKULIC 1996 quote 11.78+-0.11+-0.13 We add 0.66 to undo their correction for unseen K(L)0 and modify the systematic error accordingly.


pdgid: S035R43
text:
Not independent of ALBRECHT 1992D Gamma(mu- nubar_mu nu_tau)/Gamma(e- nubar_e nu_tau), Gamma(mu- nubar_mu nu_tau)xGamma(e- nubar_e nu_tau), and Gamma(h- >=0K0L nu_tau)/Gamma(e- nubar_e nu_tau) values.


pdgid: S035R43
text:
DECAMP 1992C quote B(h- >= 0 K0L >= 0 (K0S --> pi+ pi-) nu_tau) = 13.32+-0.44+-0.33. We subtract 0.35 to correct for their inclusion of the K(S)0 decays.


pdgid: S035R43
text:
BARTEL 1986D result for B(pi- nu_tau) with 0.59% added to remove their K- correction and adjusted for 1992 B(``1 prong'').


pdgid: S035R43
text:
BEHREND 1983C quote B(pi- nu_tau) = 9.9+-1.7+-1.3 after subtracting 1.3+-0.5 to correct for B(K- nu_tau).


pdgid: S035B73
text:
The correlation coefficients between this measurement and the ANASTASSOV 1997 measurements of B(mu nubar_mu nu_tau), B(e nubar_e nu_tau), B(mu nubar_mu nu_tau)/B(e nubar_e nu_tau), and B(h- nu_tau)/B(e nubar_e nu_tau) are 0.50, 0.48, 0.07, and 0.63 respectively.


pdgid: S035B97
text:
Not independent of AUBERT 2010F Gamma(tau- --> pi- nu_tau)/Gamma(tau- --> e- nubar_e nu_tau) and Gamma(tau- --> K- nu_tau)/Gamma(tau- --> e- nubar_e nu_tau).


pdgid: S035B97
text:
The correlation coefficients between this measurement and the ANASTASSOV 1997 measurements of B(mu nubar_mu nu_tau), B(e nubar_e nu_tau), B(mu nubar_mu nu_tau)/B(e nubar_e nu_tau), and B(h- nu_tau) are 0.08, -0.39, 0.45, and 0.63 respectively.


pdgid: S035C78
text:
See footnote to AUBERT 2010F Gamma(tau- --> mu- nubar_mu nu_tau)/Gamma(tau- --> e- nubar_e nu_tau) for correlations with other measurements.


pdgid: S035R7
text:
The correlation coefficient between this measurement and the ABBIENDI 2001J B(tau- --> K- >=0pi0 >=0K0 >=0gamma nu_tau) is 0.60.


pdgid: S035R42
text:
BURCHAT 1987 quote for B(pi+- >=1 neutral nu_tau) = 0.378+-0.012+-0.010. We add 0.006 to account for contribution from (K^*()- nu_tau) which they fixed at BR = 0.013.


pdgid: S035C01
text:
See footnote to ABDALLAH 2006A Gamma(tau- --> h- nu_tau)/Gamma(total) measurement for correlations with other measurements.


pdgid: S035R84
text:
ARTUSO 1994 reports the combined result from three independent methods, one of which (23% of the tau- -->h- pi0 nu_tau) is normalized to the inclusive one-prong branching fraction, taken as 0.854+-0.004. Renormalization to the present value causes negligible change.


pdgid: S035R84
text:
AKERS 1994E quote 26.25+-0.36+-0.52E-2; we subtract 0.27% from their number to correct for tau- --> h- K0L nu_tau.


pdgid: S035R8
text:
The authors divide by ( Gamma(3) + Gamma(5) + Gamma(9) + Gamma(10) )/Gamma = 0.467 to obtain this result.


pdgid: S035R8
text:
Experiment had no hadron identification. Kaon corrections were made, but insufficient information is given to permit their removal.


pdgid: S035R19
text:
BEHREND 1984 assume a flat nonresonant mass distribution down to the rho(770) mass, using events with mass above 1300 to set the level.


pdgid: S035B74
text:
BUSKULIC 1996 quote 9.29+-0.13+-0.10. We add 0.19 to undo their correction for tau- --> h- K0 nu_tau.


pdgid: S035R20
text:
PROCARIO 1993 entry is obtained from B(h- 2pi0 nu_tau)/B(h- pi0 nu_tau) using ARTUSO 1994 result for B(h- pi0 nu_tau).


pdgid: S035B21
text:
PROCARIO 1993 quote 0.345+-0.006+-0.016 after correction for 2 kaon backgrounds assuming B(K^*()- nu_tau)=1.42+-0.18% and B(h- K0 pi0 nu_tau)=0.48+-0.48%. We multiply by 0.990+-0.010 to remove these corrections to B(h- pi0 nu_tau).


pdgid: S035C48
text:
Model-independent limit from structure function analysis on contribution to B(tau- --> pi- 2pi0 nu_tau (ex. K0)) from scalars.


pdgid: S035C49
text:
Model-independent limit from structure function analysis on contribution to B(tau- --> pi- 2pi0 nu_tau (ex. K0)) from vectors.


pdgid: S035B30
text:
BATTLE 1994 quote 14+-10+-3E-4 or <30E-4 at 90% CL. We subtract 5+-2E-4 to account for tau- --> K- (K0 --> pi0 pi0) nu_tau background.


pdgid: S035R21
text:
PROCARIO 1993 entry is obtained from B(h- 3pi0 nu_tau)/B(h- pi0 nu_tau) using ARTUSO 1994 result for B(h- pi0 nu_tau).


pdgid: S035R21
text:
BUSKULIC 1996 quote B(h- 3pi0 nu_tau (ex. K0)) = 1.17+-0.09+-0.11. We add 0.07 to remove their correction for K0 backgrounds.


pdgid: S035R21
text:
Highly correlated with GAN 1987 G(tau- --> eta pi- pi0 nu_tau)/G(total) value. Authors quote B(pi+- 3pi0 nu_tau) + 0.67B(pi+- eta pi0 nu_tau) = 0.047+-0.010+-0.011.


pdgid: S035B22
text:
PROCARIO 1993 quote 0.041+-0.003+-0.005 after correction for 2 kaon backgrounds assuming B(K^*()- nu_tau)=1.42+-0.18% and B(h- K0 pi0 nu_tau)=0.48+-0.48%. We add 0.003+-0.003 and multiply the sum by 0.990+-0.010 to remove these corrections.


pdgid: S035B31
text:
BUSKULIC 1994E quote B(K- >= 0pi0 >= 0K0 nu_tau) - [B(K- nu_tau) + B(K- pi0 nu_tau) + B(K- K0 nu_tau) + B(K- pi0 pi0 nu_tau) + B(K- pi0 K0 nu_tau)] = 5+-13E-4 accounting for common systematic errors in BUSKULIC 1994E and BUSKULIC 1994F measurements of these modes. We assume B(K- >= 2K0 nu_tau) and B(K- >= 4pi0 nu_tau) are negligible.


pdgid: S035B79
text:
PROCARIO 1993 quotes B(h- 4pi0 nu_tau)/B(h- pi0 nu_tau) =0.006+-0.002+-0.002. We multiply by the ARTUSO 1994 result for B(h- pi0 nu_tau) to obtain B(h- 4pi0 nu_tau). PROCARIO 1993 assume B(h- >=5 pi0 nu_tau) is small and do not correct for it.


pdgid: S035B79
text:
BUSKULIC 1996 quote result for tau- --> h- >= 4pi0 nu_tau. We assume B(h- >= 5pi0 nu_tau) is negligible.


pdgid: S035R26
text:
The correlation coefficient between this measurement and the ABBIENDI 2001J B(tau- --> K- nu_tau) is 0.60.


pdgid: S035R26
text:
BATTLE 1994 quote 1.60+-0.12+-0.19. We add 0.10+-0.02 to correct for their rejection of K0S --> pi+ pi- decays.


pdgid: S035R26
text:
Not independent of BARATE 1999K B(K- nu_tau), B(K- pi0 nu_tau), B(K- 2pi0 nu_tau (ex. K0)), B(K- 3pi0 nu_tau (ex. K0)), B(K- K0 nu_tau), and B(K- K0 pi0 nu_tau) values.


pdgid: S035R26
text:
Not independent of BUSKULIC 1996 B(K- nu_tau), B(K- pi0 nu_tau), B(K- 2pi0 nu_tau), B(K- K0 nu_tau), and B(K- K0 pi0 nu_tau) values.


pdgid: S035R27
text:
Not independent of ABBIENDI 2001J B(tau- --> K- nu_tau) and B(tau- --> K- >=0pi0 >=0K0 >=0gamma nu_tau) values.


pdgid: S035B43
text:
Not independent of RYU 2014 measurements of B(tau- --> pi- Kbar0 nu_tau), B(tau- --> K- K0 nu_tau), B(tau- --> pi- Kbar0 pi0 nu_tau), B(tau- --> K- K0 pi0 nu_tau), B(tau- --> pi- K0S K0S nu_tau), and B(tau- --> pi- K0S K0S pi0 nu_tau).


pdgid: S035B32
text:
BARATE 1998E reconstruct K0's using K0S --> pi+ pi- decays. Not independent of BARATE 1998E B(K0 particles^- nu_tau) value.


pdgid: S035B52
text:
EPIFANOV 2007 quote B(tau- --> K^*(892)- nu_tau) B(K^*(892)- --> KS pi-) / B(tau- --> KS pi- nu_tau) = 0.933+-0.027. We multiply their B(tau- --> Kbar0 pi- nu_tau) by [1-(0.933+-0.027)] to obtain this result.


pdgid: S035B68
text:
Not independent of BARATE 1998E B(tau- --> pi- Kbar0 pi0 tau) and B(tau- --> K- K0 pi0 nu_tau) values.


pdgid: S035C10
text:
BARATE 1999K measure K0's by detecting K(L)0's in hadron calorimeter. They determine the Kbar0 rho- fraction in tau- --> pi- Kbar0 pi0 nu_tau decays to be (0.72+-0.12+-0.10) and multiply their B(pi- Kbar0 pi0 nu_tau) measurement by this fraction to obtain the quoted result.


pdgid: S035C10
text:
BARATE 1998E reconstruct K0's using K0S --> pi+ pi- decays. They determine the Kbar0 rho- fraction in tau- --> pi- Kbar0 pi0 nu_tau decays to be (0.64+-0.09+-0.10) and multiply their B(pi- Kbar0 pi0 nu_tau) measurement by this fraction to obtain the quoted result.


pdgid: S035B51
text:
BARATE 1998E obtain this value by adding twice their B(pi- K0S K0S nu_tau) value to their B(pi- K0S K0L nu_tau) value.


pdgid: S035B69
text:
The correlation coefficient between this measurement and the LEES 2012Y G(tau- --> pi- K0S K0S pi0 nu_tau)/G(total) one is 0.0828.


pdgid: S035C44
text:
BARATE 1999R combine BARATE 1998E Gamma(pi- K0S K0S pi0 nu_tau)/Gamma(total) and Gamma(pi- K0S K0L pi0 nu_tau)/Gamma(total) measurements to obtain this value.


pdgid: S035C2
text:
The correlation coefficient between this measurement and the LEES 2012Y G(tau- --> pi- K0S K0S nu_tau)/G(total) one is 0.0828.


pdgid: S035R31
text:
Not independent of BERGER 1985 G(tau- --> mu- nubar_mu nu_tau)/G(total), [G(tau- --> e- nubar_e nu_tau)/G(total), [G(tau- --> h- >=1 neutrals nu_tau)/G(total), and [G(tau- --> h- >=0K0L nu_tau)/G(total), and therefore not used in the fit.


pdgid: S035R31
text:
Low energy experiments are not in average or fit because the systematic errors in background subtraction are judged to be large.


pdgid: S035B63
text:
The correlation coefficients between this measurement and the ACHARD 2001D measurements of B(tau --> ``1-prong'') and B(tau --> ``5-prong'') are -0.978 and -0.19 respectively.


pdgid: S035B63
text:
The correlation coefficients between this measurement and the ABREU 2001M measurements of B(tau --> 1-prong) and B(tau --> 5-prong) are -0.98 and -0.08 respectively.


pdgid: S035B63
text:
Not independent of BALEST 1995C B(h- h- h+ nu_tau) and B(h- h- h+ pi0 nu_tau) values, and BORTOLETTO 1993 B(h- h- h+ 2pi0 nu_tau)/B(h- h- h+ >=0 neutrals nu_tau) value.


pdgid: S035B63
text:
This ALBRECHT 1992D value is not independent of their Gamma(mu- nubar_mu nu_tau)Gamma(e- nubar_e nu_tau)/Gamma(total)**2 value.


pdgid: S035R28
text:
ALBRECHT 1996E not independent of ALBRECHT 1993C Gamma(h- h- h+ nu_tau (ex. K0)xGamma(particle^->=0 neutrals >=0 K0L nu_tau)/Gamma(total)**2 value.


pdgid: S035R28
text:
BUSKULIC 1996 quote B(h- h- h+ nu_tau (ex. K0)) = 9.50+-0.10+-0.11. We add 0.42 to remove their K0 correction and reduce the systematic error accordingly.


pdgid: S035R28
text:
BEHREND 1990 subtract 0.3% to account for the tau- --> K^*(892)- nu_tau contribution to measured events.


pdgid: S035R28
text:
Value obtained by multiplying paper's R = B(h- h- h+ nu_tau)/B(3-prong) by B(3-prong) = 0.143 and subtracting 0.3% for K^*(892) background.


pdgid: S035B62
text:
Not independent of AKERS 1995Y B(h- h- h+ >=0 neutrals nu_tau (ex. K0S --> pi+ pi-)) and B(h- h- h+ nu_tau (ex. K0))/B(h- h- h+ >=0 neutrals nu_tau (ex. K0S --> pi+ pi-)) values.


pdgid: S035C19
text:
47% correlated with BRIERE 2003 tau- --> K- pi+ pi- nu_tau and 71% correlated with tau- --> K- K+ pi- nu_tau because of a common 5% normalization error.


pdgid: S035C50
text:
Model-independent limit from structure function analysis on contribution to B(tau- --> pi- pi+ pi- nu_tau (ex. K0)) from non-axial vectors.


pdgid: S035R30
text:
ALBRECHT 1987L measure the product of branching ratios B(3pi+- pi0 nu_tau) B((e nubar or mu nubar or pi or K or rho ) nu_tau) = 0.029 and use the PDG 1986 values for the second branching ratio which sum to 0.69+-0.03 to get the quoted value.


pdgid: S035R30
text:
Contributions from kaons and from >1pi0 are subtracted. Not independent of (3-prong + 0pi0) and (3-prong + >=0pi0) values.


pdgid: S035B78
text:
Not independent of AKERS 1995Y B(h- h- h+ >=0 neutrals nu_tau (ex. K0S --> pi+ pi-)) and B(h- h- h+ >=0 neutrals nu_tau (ex. K0))/B(h- h- h+ >=0 neutrals nu_tau (ex. K0S --> pi+ pi-)) values.


pdgid: S035B76
text:
BUSKULIC 1996 quote B(h- h- h+ pi0 nu_tau (ex. K0)) = 4.30+-0.09+-0.09. We add 0.15 to remove their K0 correction and reduce the systematic error accordingly.


pdgid: S035C23
text:
SCHAEL 2005C quote (4.590+-0.057+-0.064)%. We add 0.008% to remove their correction for tau- --> pi- pi0 omega nu_tau --> pi- pi0 pi+ pi- nu_tau decays. See footnote to SCHAEL 2005C Gamma(tau- --> e- nubar_e nu_tau)/Gamma(total) measurement for correlations with other measurements.


pdgid: S035B59
text:
SCHAEL 2005C quote (0.392+-0.030+-0.035)%. We add 0.043% to remove their correction for tau- --> pi- eta pi0 nu_tau --> pi- pi+ pi- 2pi0 nu_tau and tau- --> K^*(892)- eta nu_tau --> K- pi+ pi- 2pi0 nu_tau decays. See footnote to SCHAEL 2005C Gamma(tau- --> e- nubar_e nu_tau)/Gamma(total) measurement for correlations with other measurements.


pdgid: S035B57
text:
BUSKULIC 1996 state their measurement is for B(h- h- h+ >=3 pi0 nu_tau). We assume that B(h- h- h+ >= 4pi0 nu_tau) is very small.


pdgid: S035C85
text:
Not independent of LEES 2012X Gamma(tau- --> eta pi- pi+ pi- nu_tau (ex.K0))/Gamma, Gamma(tau- --> eta pi- pi0 pi0 nu_tau)/Gamma, Gamma(tau- --> pi- omega 2pi0 nu_tau)/Gamma, and Gamma(tau- --> f_1(1285) pi- nu_tau --> eta pi- pi+ pi- nu_tau)/Gamma values.


pdgid: S035R41
text:
We multiply 0.58% by 0.20, the relative systematic error quoted by BAUER 1994, to obtain the systematic error.


pdgid: S035R41
text:
Error correlated with MILLS 1985 (K K pi nu) value. We multiply 0.22% by 0.23, the relative systematic error quoted by MILLS 1985, to obtain the systematic error.


pdgid: S035C40
text:
Not independent of BARATE 1998 Gamma(tau- --> K- pi+ pi- nu_tau)/Gamma(total) and Gamma(tau- --> K- pi+ pi- pi0 nu_tau)/Gamma(total) values.


pdgid: S035C21
text:
See footnote to LEE 2010 Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0))/Gamma(total) measurement for correlations with other measurements. Not independent of LEE 2010 Gamma(tau- --> K- pi+ pi- nu_tau (ex.K0))/Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0)) value.


pdgid: S035C21
text:
See footnote to AUBERT 2008 Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0))/Gamma(total) measurement for correlations with other measurements.


pdgid: S035C21
text:
47% correlated with BRIERE 2003 tau- --> pi- pi+ pi- nu_tau and 34% correlated with tau- --> K- K+ pi- nu_tau because of a common 5% normalization error.


pdgid: S035C21
text:
Not independent of RICHICHI 1999 Gamma(tau- --> K- h+ pi- nu_tau (ex.K0))/Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0)), Gamma(tau- --> K- K+ pi- nu_tau)/Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0)) and BALEST 1995C Gamma(tau- --> h- h- h+ nu_tau (ex.K0))/Gamma(total) values.


pdgid: S035C76
text:
Not independent of LEE 2010 Gamma(tau- --> K- pi+ pi- nu_tau (ex.K0))/Gamma(total) and Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0))/Gamma(total) values.


pdgid: S035C52
text:
ASNER 2000B assume tau- --> K- pi+ pi- nu_tau (ex. K0) decays proceed only through K rho and K^* pi intermediate states. They assume the resonance structure of tau- --> K- pi+ pi- nu_tau (ex. K0) decays is dominated by K_{{1}}(1270)- and K_{{1}}(1400)- resonances, and assume B(K_1(1270) --> K^*(892) pi) = (16+-5)%, B(K_1(1270) --> K rho) = (42+-6)%, and B(K_1(1400) --> K rho) = 0.


pdgid: S035C52
text:
BARATE 1999R assume tau- --> K- pi+ pi- nu_tau (ex. K0) decays proceed only through K rho and K^* pi intermediate states. The quoted error is statistical only.


pdgid: S035C25
text:
Not independent of ARMS 2005 Gamma(tau- --> K- pi+ pi- pi0 nu_tau (ex.K0,omega)) / Gamma(total) and Gamma(tau- --> K- omega nu_tau) / Gamma(total) values.


pdgid: S035B37
text:
We multiply 0.15% by 0.20, the relative systematic error quoted by BAUER 1994, to obtain the systematic error.


pdgid: S035B37
text:
Not independent of BARATE 1998 Gamma(tau- --> K- K+ pi- nu_tau)/Gamma(total) and Gamma(tau- --> K- K+ pi- pi0 nu_tau)/Gamma(total) values.


pdgid: S035R40
text:
See footnote to LEE 2010 Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0))/Gamma(total) measurement for correlations with other measurements. Not independent of LEE 2010 Gamma(tau- --> K- K+ pi- nu_tau)/Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0)) value.


pdgid: S035R40
text:
71% correlated with BRIERE 2003 tau- --> pi- pi+ pi- nu_tau and 34% correlated with tau --> K- pi+ pi- nu_tau because of a common 5% normalization error.


pdgid: S035R40
text:
Not independent of RICHICHI 1999 Gamma(tau- --> K- K+ pi- nu_tau)/ Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0)) and BALEST 1995C Gamma(tau- --> h- h- h+ nu_tau (ex.K0))/Gamma(total) values.


pdgid: S035R40
text:
Error correlated with MILLS 1985 (K pi pi pi0 nu) value. We multiply 0.22% by 0.23, the relative systematic error quoted by MILLS 1985, to obtain the systematic error.


pdgid: S035C35
text:
Not independent of LEE 2010 Gamma(tau- --> K- K+ pi- nu_tau)/Gamma(total) and Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0))/Gamma(total) values.


pdgid: S035C8
text:
Not independent of RICHICHI 1999 Gamma(tau- --> K- K+ pi- nu_tau)/Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0)) and BALEST 1995C Gamma(tau- --> h- h- h+ nu_tau (ex.K0))/Gamma(total) values.


pdgid: S035C9
text:
See footnote to LEE 2010 Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0))/Gamma(total) measurement for correlations with other measurements. Not independent of LEE 2010 Gamma(tau- --> K- K+ K- nu_tau)/Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0)) value.


pdgid: S035C77
text:
Not independent of LEE 2010 Gamma(tau- --> K- K+ K- nu_tau)/Gamma(total) and Gamma(tau- --> pi- pi+ pi- nu_tau (ex.K0))/Gamma(total) values.


pdgid: S035P01
text:
JIN 2019 measures B(tau- --> pi- e- e+ nu_tau ( #mass_anythingpi- e- e+ > 1.05GeV/c^2)) = 5.90+-0.53+-0.86E-6, which is only sensitive to the structure-dependent contribution, and assumes that the decay proceeds with either a pure axial-vector current or a pure vector current to obtain the two respective branching fraction measurements for this mode, which are 100% correlated.


pdgid: S035R33
text:
The correlation coefficients between this measurement and the ACHARD 2001D measurements of B(tau --> ``1-prong'') and B(tau --> ``3-prong'') are -0.082 and -0.19 respectively.


pdgid: S035R33
text:
The correlation coefficients between this measurement and the ABREU 2001M measurements of B(tau --> 1-prong) and B(tau --> 3-prong) are -0.08 and -0.08 respectively.


pdgid: S035R33
text:
Not independent of ACKERSTAFF 1999E B(tau- --> 3h- 2h+ nu_tau (ex. K0)) and B(tau- --> 3h- 2h+ pi0 nu_tau (ex. K0)) measurements.


pdgid: S035C88
text:
Not independent of LEES 2012X Gamma(tau- --> f_1(1285) pi- nu_tau --> 3pi- 2pi+ nu_tau)/Gamma and Gamma(tau- --> 3pi- 2pi+ nu_tau (ex.K0, omega, f_{{1}}(1285)))/Gamma values.


pdgid: S035R39
text:
SCHAEL 2005C quote 1.4+-0.7+-0.9E-4. We add 0.7E-4 to remove their correction for tau- --> eta pi- pi+ pi- nu_tau --> 3pi- 2pi+ pi0 nu_tau and tau- --> K^*(892)- eta nu_tau --> 3pi- 2pi+ pi0 nu_tau decays. See footnote to SCHAEL 2005C Gamma(tau- --> e- nubar_e nu_tau)/Gamma(total) measurement for correlations with other measurements.


pdgid: S035C90
text:
Not independent of LEES 2012X measurements of Gamma(tau- --> 2pi- pi+ omega nu_tau (ex.K0))/Gamma, Gamma(tau- --> eta pi- pi+ pi- nu_tau (ex.K0))/Gamma, and Gamma(tau- --> 3pi- 2pi+ pi0 nu_tau (ex.K0, eta, omega, f_{{1}}(1285)))/Gamma.


pdgid: S035C91
text:
Not independent of LEES 2012X Gamma(tau- --> 2pi- pi+ omega nu_tau (ex.K0))/Gamma and Gamma(tau- --> 3pi- 2pi+ pi0 nu_tau (ex.K0, eta, omega, f_{{1}}(1285)))/Gamma values.


pdgid: S035B45
text:
Not independent of GIBAUT 1994B B(3h- 2h+ nu_tau), PROCARIO 1993 B(h- 4pi0 nu_tau), and BORTOLETTO 1993 B(2h- h+ 2pi0 nu_tau)/B(``3prong'') measurements. Result is corrected for eta contributions.


pdgid: S035C47
text:
BARATE 1999R perform a combined analysis of all ALEPH LEP 1 data on tau branching fraction measurements for decay modes having total strangeness equal to -1.


pdgid: S035R9
text:
EPIFANOV 2007 quote B(tau- --> K^*(892)- nu_tau) B(K^*(892)- --> KS pi-) = (3.77+-0.02(stat) +-0.12(syst) +-0.12(mod))x10**-3. We add the systematic and model uncertainties in quadrature and divide by B(K^*(892)- --> KS pi-) = 0.3333.


pdgid: S035R9
text:
Not independent of COAN 1996 B(pi- Kbar0 nu_tau) and BATTLE 1994 B(K- pi0 nu_tau) measurements. K pi final states are consistent with and assumed to originate from K^*(892)- production.


pdgid: S035R9
text:
This result is obtained from their B(pi- Kbar0 nu_tau) assuming all those decays originate in K^*(892)- decays.


pdgid: S035R9
text:
BUSKULIC 1994F obtain this result from BUSKULIC 1994F B(Kbar0 pi- nu_tau) and BUSKULIC 1994E B(K- pi0 nu_tau) assuming all of those decays originate in K^*(892)- decays.


pdgid: S035B49
text:
ABREU 1994K quote B(tau- --> K^*(892)- nu_tau)B(K^*(892)- --> K- pi0)/B(tau- --> rho- nu_tau) = 0.025+-0.009. We divide by B(K^*(892)- --> K- pi0) = 0.333 to obtain this result.


pdgid: S035B60
text:
BARATE 1998 measure the K- (rho0 --> pi+ pi-) fraction in tau- --> K- pi+ pi- nu_tau decays to be (35+-11)% and derive this result from their measurement of Gamma(tau- --> K- pi+ pi- nu_tau)/Gamma(total) assuming the intermediate states are all K- rho and K- K^*(892)0.


pdgid: S035B70
text:
BARATE 1998 measure the K- K^*(892)0 fraction in tau- --> K- K+ pi- nu_tau decays to be (87+-13)% and derive this result from their measurement of Gamma(tau- --> K- K+ pi- nu_tau)/Gamma(total).


pdgid: S035C11
text:
BARATE 1999K measure K0's by detecting K(L)0's in their hadron calorimeter. They determine the Kbar0 rho- fraction in tau- --> pi- Kbar0 pi0 nu_tau decays to be (0.72+-0.12+-0.10) and multiply their B(pi- Kbar0 pi0 nu_tau) measurement by one minus this fraction to obtain the quoted result.


pdgid: S035C11
text:
BARATE 1998E reconstruct K0's using K0S --> pi+ pi- decays. They determine the Kbar0 rho- fraction in tau- --> pi- Kbar0 pi0 nu_tau decays to be (0.64+-0.09+-0.10) and multiply their B(pi- Kbar0 pi0 nu_tau) measurement by one minus this fraction to obtain the quoted result.


pdgid: S035B40
text:
We multiply 0.41% by 0.25, the relative systematic error quoted by BAUER 1994, to obtain the systematic error.


pdgid: S035B41
text:
We multiply 0.76% by 0.25, the relative systematic error quoted by BAUER 1994, to obtain the systematic error.


pdgid: S035B42
text:
We multiply 1.17% by 0.25, the relative systematic error quoted by BAUER 1994, to obtain the systematic error. Not independent of BAUER 1994 B(K_1(1270)- nu_tau) and BAUER 1994 B(K_1(1400)- nu_tau) measurements.


pdgid: S035C41
text:
ABBIENDI 2000D assume the resonance structure of tau- --> K- pi+ pi- nu_tau decays is dominated by the K_{{1}}(1270)- and K_{{1}}(1400)- resonances.


pdgid: S035C41
text:
ASNER 2000B assume the resonance structure of tau- --> K- pi+ pi- nu_tau (ex. K0) decays is dominated by K_{{1}}(1270)- and K_{{1}}(1400)- resonances.


pdgid: S035R10
text:
ACCIARRI 1995F quote B(tau- --> K^*(1430)- --> pi- Kbar0 nu_tau) <0.11%. We divide by B(K^*(1430)- --> pi- Kbar0) = 0.33 to obtain the limit shown.


pdgid: S035R78
text:
Weighted average of BERGFELD 1997 and ANASTASSOV 2001 value of 1.5+-0.6+-0.3E-4 obtained using eta's reconstructed from eta --> pi+ pi- pi0 decays.


pdgid: S035C26
text:
Not independent of INAMI 2009 B(tau- --> eta K- pi0 nu_tau) and B(tau- --> eta Kbar0 pi- nu_tau) values.


pdgid: S035C28
text:
We multiply the INAMI 2009 measurement B(tau- --> eta K0S pi- nu_tau) = 0.44+-0.07+-0.03E-4 by 2 to obtain the listed value.


pdgid: S035C28
text:
We multiply the BISHAI 1999 measurement B(tau- --> eta K0S pi- nu_tau) = 1.10+-0.35+-0.11E-4 by 2 to obtain the listed value.


pdgid: S035C73
text:
We multiply the INAMI 2009 measurement B(tau- --> eta K0S pi- pi0 nu_tau) < 2.5E-5 by 2 to obtain the listed value.


pdgid: S035C74
text:
We multiply the INAMI 2009 measurement B(tau- --> eta K- K0S nu_tau) < 4.5E-6 by 2 to obtain the listed value.


pdgid: S035B89
text:
LEES 2012X uses 468 fb**-1 of data taken at e+ e- Ecm = 10.6 GeV. It gives the average of the three measurements listed here as 2.25+-0.07+-0.12E-4.


pdgid: S035B89
text:
Weighted average of BERGFELD 1997 and ANASTASSOV 2001 measurements using eta's reconstructed from eta --> pi+ pi- pi0 and eta --> 3pi0 decays.


pdgid: S035C81
text:
LEES 2012X obtain this result by subtracting their B(tau- --> f_1(1285) pi- nu_tau --> eta pi- pi+ pi- nu_tau) measurement from their B(tau- --> eta pi- pi+ pi- nu_tau (ex.K0)) measurement.


pdgid: S035B93
text:
LEES 2012X obtain this value by dividing their B(tau- --> f_1(1285) pi- nu_tau --> 3pi- 2pi+ nu_tau) measurement by the PDG 2012 value of B(f_1(1285) --> 2pi+ 2pi-) = 0.111+0.007-0.006.


pdgid: S035B93
text:
LEES 2012X obtain this value by dividing their B(tau- --> f_1(1285) pi- nu_tau --> eta pi- pi+ pi- nu_tau) measurement by 2/3 of the PDG 2012 value of B(f_1(1285) --> eta pi pi) = 0.524+0.019-0.021.


pdgid: S035B93
text:
AUBERT 2008AE obtain this value by dividing their B(tau- --> f_1(1285) pi- nu_tau --> eta pi- pi+ pi- nu_tau) measurement by the PDG 2006 value of B(f_1(1285) --> eta pi- pi+) = 0.35+-0.11. The quote 3.19+-0.18+-0.16+-0.99E-4 where the final error is due to the uncertainty on B(f_1(1285) --> eta pi- pi+). We combine the two systematic errors in quadrature.


pdgid: S035B93
text:
AUBERT,B 2005W use the f_1(1285) --> 2pi+ 2pi- decay mode and the PDG 2004 value of B(f_1(1285) --> 2pi+ 2pi-) = 0.110+0.007-0.006.


pdgid: S035B94
text:
Not independent of AUBERT 2008AE B(tau- --> f_1(1285) pi- nu_tau --> eta pi- pi+ pi- nu_tau) and B(tau- --> eta pi- pi+ pi- nu_tau (ex.K0)) values.


pdgid: S035R14
text:
BUSKULIC 1996 quote the fraction of tau --> h- h- h+ pi0 nu_tau (ex. K0) decays which originate in a h- omega final state = 0.383+-0.029. We divide this by the omega(782) --> pi+ pi- pi0 branching fraction (0.888).


pdgid: S035R14
text:
BALEST 1995C quote the fraction of tau- --> h- h- h+ pi0 nu_tau (ex. K0) decays which originate in a h- omega final state equals 0.412+-0.014+-0.015. We divide this by the omega(782) --> pi+ pi- pi0 branching fraction (0.888).


pdgid: S035R14
text:
ALBRECHT 1991D quote the fraction of tau- --> h- h- h+ pi0 nu_tau decays which originate in a pi- omega final state equals 0.33+-0.04+-0.02. We divide this by the omega(782) --> pi+ pi- pi0 branching fraction (0.888).


pdgid: S035B26
text:
Not independent of BORTOLETTO 1993 Gamma(tau- --> h- omega pi0 nu_tau)/Gamma(tau- --> h- h- h+ 2pi0 nu_tau (ex.K0)) value.


pdgid: S035P06
text:
BRYMAN 2021 reinterprets the upper limit result on B(tau- --> e- gamma) and B(tau- --> mu- gamma) by AUBERT 2010B, estimating with a simulation the efficiency for this decay mode to be detected as the corresponding AUBERT 2010B decay mode.


pdgid: S035R55
text:
HAYRAPETYAN 2024J use 33.2 fb**-1 of data taken in 2016 and used for the same search in SIRUNYAN 2021D and 97.7 fb**-1 of data taken in 2017-2018.


pdgid: S035P11
text:
UNO 2025 limit holds for bosons with mass = 0.0 GeV. For masses between 0.0 and 1.6 GeV, the limit varies in the range (0.3 -- 6.0)xE-4.


pdgid: S035P10
text:
UNO 2025 limit holds for bosons with mass = 0.0 GeV. For masses between 0.0 and 1.6 GeV, the limit varies in the range (0.1 -- 3.3)xE-4.


pdgid: S035B11
text:
ADACHI 2023A limit holds for bosons with mass = 0.0 GeV. The limit rises to 9.7E-3 for a mass of 1.0 GeV, then falls to 1.1E-3 at the upper mass limit of 1.6 GeV.


pdgid: S035B11
text:
BRYMAN 2021 reports indirect limits obtained from the consistency of the world averages of  B(tau- --> e- nubar_e nu_tau) and B(tau- --> mu- nubar_mu nu_tau) with their Standard  Model predictions, without a simulation of the efficiency as a function of the X mass for the  searched decay modes to be detected as the corresponding Standard Model decay modes.


pdgid: S035B11
text:
ALBRECHT 1995G limit holds for bosons with mass <0.4 GeV. The limit rises to 0.036 for a mass of 1.0 GeV, then falls to 0.006 at the upper mass limit of 1.6 GeV.


pdgid: S035B11
text:
ALBRECHT 1990E limit applies for spinless boson with mass < 100 MeV, and rises to 0.050 for mass = 500 MeV.


pdgid: S035B12
text:
ADACHI 2023A limit holds for bosons with mass = 0.0 GeV. The limit rises to 12.2E-3 for a mass of 1.0 GeV, then falls to 0.7E-3 at the upper mass limit of 1.6 GeV.


pdgid: S035B12
text:
ALBRECHT 1995G limit holds for bosons with mass <1.3 GeV. The limit rises to 0.034 for a mass of 1.4 GeV, then falls to 0.003 at the upper mass limit of 1.6 GeV.


pdgid: S035B12
text:
ALBRECHT 1990E limit applies for spinless boson with mass < 100 MeV, and rises to 0.071 for mass = 500 MeV.


pdgid: S035RHO
text:
Combined fit to ARGUS tau decay parameter measurements in ALBRECHT 1998, ALBRECHT 1995C, ALBRECHT 1993G, and ALBRECHT 1994E. ALBRECHT 1998 use tau pair events of the type tau- tau+ --> (lepton- nubar_lepton nu_tau)(pi+ pi0 nubar_tau), and their charged conjugates.


pdgid: S035RHO
text:
ABE 1997O assume eta = 0 in their fit. Letting eta vary in the fit gives a rho value of 0.69+-0.13+-0.05.


pdgid: S035RHO
text:
Value is from a simultaneous fit for the rho and eta decay parameters to the lepton energy spectrum. Not independent of ALBRECHT 1990E rho(e or mu) value which assumes eta = 0. Result is strongly correlated with ALBRECHT 1995C.


pdgid: S035RHO
text:
Combined fit to ARGUS tau decay parameter measurements in ALBRECHT 1995C, ALBRECHT 1993G, and ALBRECHT 1994E.


pdgid: S035RHE
text:
ALBRECHT 1998 use tau pair events of the type tau- tau+ --> (lepton- nubar_lepton nu_tau)(pi+ pi0 nubar_tau), and their charged conjugates.


pdgid: S035RHE
text:
ALBRECHT 1995 use tau pair events of the type tau- tau+ --> (lepton- nubar_lepton nu_tau) (h+ h- h+ (pi0) nubar_tau) and their charged conjugates.


pdgid: S035RHE
text:
ALBRECHT 1993G use tau pair events of the type tau- tau+ --> (mu- nubar_mu nu_tau) (e+ nu_e nubar_tau) and their charged conjugates.


pdgid: S035XI
text:
ABE 1997O assume eta = 0 in their fit. Letting eta vary in the fit gives a xi value of 1.02+-0.36+-0.05.


pdgid: S035XI
text:
Combined fit to ARGUS tau decay parameter measurements in ALBRECHT 1995C, ALBRECHT 1993G, and ALBRECHT 1994E. ALBRECHT 1995C uses events of the type tau- tau+ --> (lepton- nubar_lepton nu_tau) (h+ h- h+ nubar_tau) and their charged conjugates.


pdgid: S035XI
text:
ALBRECHT 1993G measurement determines |xi| for the case xi(e) = xi(mu), but the authors point out that other LEP experiments determine the sign to be positive.


pdgid: S035ETM
text:
ACKERSTAFF 1999D result is dominated by a constraint on eta from the OPAL measurements of the tau lifetime and B(tau- --> mu- nubar_mu nu_tau) assuming lepton universality for the total coupling strength.


pdgid: S035DXI
text:
ABE 1997O assume eta = 0 in their fit. Letting eta vary in the fit gives a (deltaxi) value of 0.87+-0.27+-0.04.


pdgid: S035XRH
text:
ALBRECHT 1994E measure the square of this quantity and use the sign determined by ALBRECHT 1990I to obtain the quoted result.


pdgid: S035XA1
text:
HEISTER 2001E quote 1.000+-0.016+-0.013+-0.020 where the errors are statistical, systematic, and an uncertainty due to the final state model. We combine the systematic error and model uncertainty.


pdgid: S035XA1
text:
ACKERSTAFF 1997R obtain this result with a model independent fit to the hadronic structure functions. Fitting with the model of Kuhn and Santamaria (ZPHY C48, 445 (1990)) gives 0.87+-0.16+-0.04, and with the model of of Isgur et al. (PR D39,1357 (1989)) they obtain 1.20+-0.21+-0.14.


pdgid: S035XA1
text:
AKERS 1995P obtain this result with a model independent fit to the hadronic structure functions. Fitting with the model of Kuhn and Santamaria (ZPHY C48, 445 (1990)) gives 0.87+-0.27+0.05-0.06, and with the model of of Isgur et al. (PR D39,1357 (1989)) they obtain 1.10+-0.31+0.13-0.14.


pdgid: S035XAL
text:
HEISTER 2001E quote 0.992+-0.007+-0.006+-0.005 where the errors are statistical, systematic, and an uncertainty due to the final state model. We combine the systematic error and model uncertainty. They use tau --> pi nu_tau, tau --> K nu_tau, tau --> rho nu_tau, and tau --> a_1 nu_tau decays.


pdgid: S035XAL
text:
ALBRECHT 1994E measure the square of this quantity and use the sign determined by ALBRECHT 1990I to obtain the quoted result. Uses tau --> a_1 nu_tau decays. Replaced by ALBRECHT 1995C.


pdgid: S035BEM
text:
SHIMIZU 2018A measurement procedure fits a distribution affected by etabar(mu), xikappa(mu) and eta^''(mu), floating etabar(mu) and xikappa(mu) and fixing eta^''(mu) = 0. The contribution of eta^''(mu) is suppressed by mass(mu)/mass(tau).


pdgid: S035XIK
text:
SHIMIZU 2018A measurement procedure fits a distribution of radiative tau decays into both  electrons and muons affected by etabar(e or mu), xikappa(e or  mu) and eta^''(e or mu), floating etabar(e or mu) and  xikappa(e or mu) and fixing eta^''(e or mu) = 0. The  contribution of eta^''(e or mu) is suppressed by mass(e)/mass(tau) for tau decaying to electrons and by mass(mu)/mass(tau) for tau decaying to muons.


pdgid: S035XKE
text:
SHIMIZU 2018A measurement procedure fits a distribution affected by etabar(e), (xikappa)(e) and eta^''(e), floating (xikappa)(e) and fixing etabar(e) = 0 and eta^''(e) = 0. The contribution of eta^''(e) is suppressed by mass(e)/mass(tau).


pdgid: S025MS
text:
The AHMED 1994 limits are from a search for neutral and charged sequential heavy leptons at HERA via the decay channels L- --> e gamma, L- --> nu W-, L- --> e Z; and L0 --> nu gamma, L0 --> e- W+, L- --> nu Z, where the W decays to lepton nu_lepton, or to jets, and Z decays to lepton+ lepton- or jets.


pdgid: S025MS
text:
RILES 1990 limits were the result of a special analysis of the data in the case where the mass difference mass(L-)-mass(L0) was allowed to be quite small, where L0 denotes the neutrino into which the sequential charged lepton decays. With a slightly reduced mass(L+-) range, the mass difference extends to about 4 GeV.


pdgid: S025MS
text:
STOKER 1989 (Mark II at PEP) gives bounds on charged heavy lepton (L+) mass for the generalized case in which the corresponding neutral heavy lepton (L0) in the SU(2) doublet is not of negligible mass.


pdgid: S025MS
text:
ABE 1988 search for L+ and L- --> hadrons looking for acoplanar jets. The bound is valid for mass(nu) < 10 GeV.


pdgid: S025MS
text:
ADACHI 1988B search for hadronic decays giving acoplanar events with large missing energy. E(cm)**ee = 52 GeV.


pdgid: S025MS
text:
ADEVA 1985 analyze one-isolated-muon data and sensitive to tau <10 nanosec. Assume B(lepton) = 0.30. Ecm = 40-47 GeV.


pdgid: S025MS
text:
AZIMOV 1980 estimated probabilities for M + N type events in e+ e- --> L+ L- deducing semi-hadronic decay multiplicities of L from e+ e- annihilation data at Ecm = (2/3)*mass(L). Obtained above limit comparing these with e+ e- data (BRANDELIK 1980).


pdgid: S025MSS
text:
ADACHI 1990C put lower limits on the mass of stable charged particles with electric charge Q satisfying 2/3 < Q/e < 4/3 and with spin 0 or 1/2. We list here the special case for a stable charged heavy lepton.


pdgid: S025MLL
text:
BUSHNIN 1973 is SERPUKHOV 70 GeV p experiment. Masses assume mean life above 7E-10 and 3E-8 respectively. Calculated from cross section (see ``Charged Quasi-Stable Lepton Production Differential Cross Section'' below) and 30 GeV muon pair production data.


pdgid: S025MDC
text:
CLARK 1981 is FNAL experiment with 209 GeV muons. Bounds apply to mu_{{P}} which couples with full weak strength to muon. See also section on ``Doubly-Charged Lepton Production Cross Section.''


pdgid: S025DB
text:
CLARK 1981 is FNAL experiment with 209 GeV muon. Looked for mu+ nucleon --> mubar_P()0 X, mubar_P()0 --> mu+ mu- nubar_mu and mu+ n --> mu_P()++ X, mu_P()++ --> 2mu+ nu_mu. Above limits are for sigmaxBR taken from their mass-dependence plot figure 2.


pdgid: S066MAE
text:
AKER 2025A use data collected by the KATRIN experiment, a precision analysis of the Tritium beta spectrum, to formulate a bound on the neutrino mass. The combined analysis of 7 science runs is reported. Supersedes AKER 2019 and AKER 2022.


pdgid: S066MAE
text:
ESFAHANI 2023 report the first continuous-spectrum measurement of H3 beta decay, using cyclotron radiation emission spectroscopy (CRES) and a small demonstration detector. The energy resolution at the endpoint is demonstrated using **83mKr and a kinematical neutrino mass limit derived from the spectral shape. A frequentist analysis obtained a limit of <152 eV.


pdgid: S066MAE
text:
AKER 2022 derive an upper limit on the kinematical neutrino mass using Tritium beta-decay and the KATRIN spectrometer. The constraint is based on combining the first two science runs.   Supersedes AKER 2019.


pdgid: S066MAE
text:
AKER 2019 report a neutrino mass limit, derived from the first month of data collected by the KATRIN tritium endpoint experiment. The analysis of the electron kinematics shows no evidence  for  neutrino mass. The quoted result is based on a frequentist analysis of the data following  the method described in LOKHOV 2015. Using the method of  Feldman and Cousins, the derived  upper limit is < 0.8 eV at 90% C.L. Superseded by AKER 2022.


pdgid: S066MAE
text:
ASEEV 2011 report the analysis of the entire beta endpoint data, taken with the Troitsk integrating electrostatic spectrometer between 1997 and 2002 (some of the earlier runs were rejected), using a windowless gaseous tritium source. The fitted value of mass(nu), based on the method of Feldman and Cousins, is obtained from the upper limit of the fit for mass**2(nu). Previous analysis problems were resolved by careful monitoring of the tritium gas column density. Supersedes LOBASHEV 1999 and BELESEV 1995.


pdgid: S066MAE
text:
KRAUS 2005 is a continuation of the work reported in WEINHEIMER 1999. This result represents the final analysis of data taken from 1997 to 2001. Various sources of systematic uncertainties have been identified and quantified. The background has been reduced compared to the initial running period. A spectral anomaly at the endpoint, reported in LOBASHEV 1999, was not observed.


pdgid: S066MAE
text:
ARNABOLDI 2003A et al. report kinematical neutrino mass limit using beta-decay of Re187. Bolometric AgReO(4) micro-calorimeters are used. Mass bound is substantially weaker than those derived from tritium beta-decays but has different systematic uncertainties.


pdgid: S066MAE
text:
LOBASHEV 1999 report a new measurement which continues the work reported in BELESEV 1995. This limit depends on phenomenological fit parameters used to derive their best fit to mass**2(nu), making unambiguous interpretation difficult. See the footnote under ``nubar Mass Squared.''


pdgid: S066MAE
text:
WEINHEIMER 1999 presents two analyses which exclude the spectral anomaly and result in an acceptable mass**2(nu). We report the most conservative limit, but the other is nearly the same. See the footnote under ``nubar Mass Squared.''


pdgid: S066MAE
text:
BELESEV 1995 (Moscow) use an integral electrostatic spectrometer with adiabatic magnetic collimation and a gaseous tritium sources. A fit to a normal Kurie plot above 18300 -- 18350 eV (to avoid a low-energy anomaly) plus a monochromatic line 7 -- 15 eV below the endpoint yields mass**2(nu) = -4.1+-10.9 eV**2, leading to this Bayesian limit.


pdgid: S066MAE
text:
CHING 1995 quotes results previously given by SUN 1993; no experimental details are given. A possible explanation for consistently negative values of mass**2(nu) is given.


pdgid: S066MAE
text:
HIDDEMANN 1995 (Munich) experiment uses atomic tritium embedded in a metal-dioxide lattice. Bayesian limit calculated from the weighted mean mass**2(nu) = 221+-4244 eV**2 from the two runs listed below.


pdgid: S066MAE
text:
STOEFFL 1995 (LLNL) result is the Bayesian limit obtained from the mass**2(nu) errors given below but with mass**2(nu) set equal to 0. The anomalous endpoint accumulation leads to a value of mass**2(nu) which is negative by more than 5 standard deviations.


pdgid: S066MAE
text:
WEINHEIMER 1993 (Mainz) is a measurement of the endpoint of the tritium beta spectrum using an electrostatic spectrometer with a magnetic guiding field. The source is molecular tritium frozen onto an aluminum substrate.


pdgid: S066MAE
text:
HOLZSCHUH 1992B (Zurich) result is obtained from the measurement mass**2(nu) = -24+-48+-61 (1sigma errors), in eV**2, using the PDG prescription for conversion to a limit in mass(nu).


pdgid: S066MAE
text:
KAWAKAMI 1991 (Tokyo) experiment uses tritium-labeled arachidic acid. This result is the Bayesian limit obtained from the mass**2(nu) limit with the errors combined in quadrature. This was also done in ROBERTSON 1991, although the authors report a different procedure.


pdgid: S066MAE
text:
ROBERTSON 1991 (LANL) experiment uses gaseous molecular tritium. The result is in strong disagreement with the earlier claims by the ITEP group [LUBIMOV 1980, BORIS 1987 (+ BORIS 1988 erratum)] that mass(nu) lies between 17 and 40 eV. However, the probability of a positive m**2 is only 3% if statistical and systematic error are combined in quadrature.


pdgid: S066M2E
text:
AKER 2025A use data collected by the KATRIN experiment, a precision analysis of the Tritium beta spectrum, to formulate a bound on the squared neutrino mass. The combined analysis of 7 science runs is reported. Supersedes AKER 2019 and AKER 2022.


pdgid: S066M2E
text:
ASEEV 2011 report the analysis of the entire beta endpoint data, taken with the Troitsk integrating electrostatic spectrometer between 1997 and 2002, using a windowless gaseous tritium source. The analysis does not use the two additional fit parameters (see LOBASHEV 99) for a step-like structure near the endpoint. Using only the runs where the tritium gas column density was carefully monitored the need for such parameters was eliminated. Supersedes LOBASHEV 1999 and BELESEV 1995.


pdgid: S066M2E
text:
KRAUS 2005 is a continuation of the work reported in WEINHEIMER 1999. This result represents the final analysis of data taken from 1997 to 2001. Problems with significantly negative squared neutrino masses, observed in some earlier experiments, have been resolved in this work.


pdgid: S066M2E
text:
AKER 2022 report results from the analysis of the Tritium beta spectrum using the combined data set collected by the KATRIN experiment in the first two science runs. Supersedes AKER 2019.


pdgid: S066M2E
text:
AKER 2019 use the first month of data collected by the KATRIN experiment to determine  mass**2(nu). The result is consistent with a neutrino mass of zero and is used to place a limit on  mass(nu). Superseded by AKER 2022.


pdgid: S066M2E
text:
LOBASHEV 1999 report a new measurement which continues the work reported in BELESEV 1995. The data were corrected for electron trapping effects in the source, eliminating the dependence of the fitted neutrino mass on the fit interval. The analysis assuming a pure beta spectrum yields significantly negative fitted mass**2(nu)~~-(20 -- 10) eV**2. This problem is attributed to a discrete spectral anomaly of about 6E-11 intensity with a time-dependent energy of 5 -- 15 eV below the endpoint. The data analysis accounts for this anomaly by introducing two extra phenomenological fit parameters resulting in a best fit of mass**2(nu)=-1.9+-3.4+-2.2 eV**2 which is used to derive a neutrino mass limit. However, the introduction of phenomenological fit parameters which are correlated with the derived mass**2(nu) limit makes unambiguous interpretation of this result difficult.


pdgid: S066M2E
text:
WEINHEIMER 1999 is a continuation of the work reported in WEINHEIMER 1993. Using a lower temperature of the frozen tritium source eliminated the dewetting of the T(2) film, which introduced a dependence of the fitted neutrino mass on the fit interval in the earlier work. An indication for a spectral anomaly reported in LOBASHEV 1999 has been seen, but its time dependence does not agree with LOBASHEV 1999. Two analyses, which exclude the spectral anomaly either by choice of the analysis interval or by using a particular data set which does not exhibit the anomaly, result in acceptable mass**2(nu) fits and are used to derive the neutrino mass limit published by the authors. We list the most conservative of the two.


pdgid: S066M2E
text:
BELESEV 1995 (Moscow) use an integral electrostatic spectrometer with adiabatic magnetic collimation and a gaseous tritium sources. This value comes from a fit to a normal Kurie plot above 18300 -- 18350 eV (to avoid a low-energy anomaly), including the effects of an apparent peak 7 -- 15 eV below the endpoint.


pdgid: S066M2E
text:
HIDDEMANN 1995 (Munich) experiment uses atomic tritium embedded in a metal-dioxide lattice. They quote measurements from two data sets.


pdgid: S066M2E
text:
STOEFFL 1995 (LLNL) uses a gaseous source of molecular tritium. An anomalous pileup of events at the endpoint leads to the negative value for mass**2(nu). The authors acknowledge that ``the negative value for the best fit of mass**2(nu) has no physical meaning'' and discuss possible explanations for this effect.


pdgid: S066M2E
text:
ROBERTSON 1991 (LANL) experiment uses gaseous molecular tritium. The result is in strong disagreement with the earlier claims by the ITEP group [LUBIMOV 1980, BORIS 1987 (+ BORIS 1988 erratum)] that mass(nu) lies between 17 and 40 eV. However, the probability of a positive mass**2(nu) is only 3% if statistical and systematic error are combined in quadrature.


pdgid: S066MNE
text:
ALPERT 2025 report a kinematical neutrino mass limit, derived from observing 6E7 Ho163 EC-decays. The HOLMES bolometric micro-calorimeter array is used. The limit is obtained by means of a Bayesian analysis. The quoted 90% is for Credibility, not Confidence Level.


pdgid: S066MNM
text:
ASSAMAGAN 1996 measurement of p_{{mu}} from pi+ --> mu+ nu at rest combined with JECKELMANN 1994 Solution B pion mass yields mass**2(nu) = -0.016+-0.023 with corresponding Bayesian limit listed above. If Solution A is used, mass**2(nu) = -0.143+-0.024 MeV**2. Replaces ASSAMAGAN 1994.


pdgid: S066MNM
text:
DOLGOV 1995 removes earlier assumptions (DOLGOV 1993) about thermal equilibrium below T(QCD) for wrong-helicity Dirac neutrinos (ENQVIST 1993, FULLER 1991) to set more stringent limits.


pdgid: S066MNM
text:
ENQVIST 1993 bases limit on the fact that thermalized wrong-helicity Dirac neutrinos would speed up expansion of early universe, thus reducing the primordial abundance. FULLER 1991 exploits the same mechanism but in the older calculation obtains a larger production rate for these states, and hence a lower limit. Neutrino lifetime assumed to exceed nucleosynthesis time, ~1 s.


pdgid: S066MNT
text:
BARATE 1998F result based on kinematics of 2939 tau- --> 2pi- pi+ nu_tau and 52 tau- --> 3pi- 2pi+ (pi0) nu_tau decays. If possible 2.5% excited a_{{1}} decay is included in 3-prong sample analysis, limit increases to 19.2 MeV.


pdgid: S066MNT
text:
ACKERSTAFF 1998T use tau --> 5pi+- nu_tau decays to obtain a limit of 43.2 MeV (95%CL). They combine this with ALEXANDER 1996M value using tau --> 3h+- nu_tau decays to obtain quoted limit.


pdgid: S066MNT
text:
AMMAR 1998 limit comes from analysis of tau- --> 3pi- 2pi+ nu_tau and tau- --> 2pi- pi+ 2pi0 nu_tau decay modes.


pdgid: S066MNT
text:
ANASTASSOV 1997 derive limit by comparing their mass(tau) measurement (which depends on mass(nu_{{tau}})) to BAI 1996 mass(tau) threshold measurement.


pdgid: S066MNT
text:
FIELDS 1997 limit for a Dirac neutrino. For a Majorana neutrino the mass region <0.93 or >31 MeV is excluded. These bounds assume N(nu)<4 from nucleosynthesis; a wider excluded region occurs with a smaller N(nu) upper limit.


pdgid: S066MNT
text:
SWAIN 1997 derive their limit from the Standard Model relationships between the tau mass, lifetime, branching fractions for tau- --> e- nubar_e nu_tau, tau- --> mu- nubar_mu nu_tau, tau- --> pi- nu_tau, and tau- --> K- nu_tau, and the muon mass and lifetime by assuming lepton universality and using world average values. Limit is reduced to 48 MeV when the CLEO tau mass measurement (BALEST 1993) is included; see CLEO's more recent mass(nu_{{tau}}) limit (ANASTASSOV 1997). Consideration of mixing with a fourth generation heavy neutrino yields sin**2(theta_{{L}})<0.016 (95%CL).


pdgid: S066MNT
text:
ALEXANDER 1996M bound comes from analyses of tau- --> 3pi- 2pi+ nu_tau and tau- --> h- h- h+ nu_tau decays.


pdgid: S066MNT
text:
BOTTINO 1996 assumes three generations of neutrinos with mixing, finds consistency with massless neutrinos with no mixing based on 1995 data for masses, lifetimes, and leptonic partial widths.


pdgid: S066MNT
text:
HANNESTAD 1996C limit is on the mass of a Majorana neutrino. This bound assumes N(nu)<4 from nucleosynthesis. A wider excluded region occurs with a smaller N(nu) upper limit. This paper is the corrected version of HANNESTAD 1996; see the erratum: HANNESTAD 1996B.


pdgid: S066MNT
text:
SOBIE 1996 derive their limit from the Standard Model relationship between the tau mass, lifetime, and leptonic branching fraction, and the muon mass and lifetime, by assuming lepton universality and using world average values.


pdgid: S066MNT
text:
BUSKULIC 1995H bound comes from a two-dimensional fit of the visible energy and invariant mass distribution of tau --> 5pi (pi0) nu_tau decays. Replaced by BARATE 1998F.


pdgid: S066MNT
text:
DOLGOV 1995 removes earlier assumptions (DOLGOV 1993) about thermal equilibrium below T(QCD) for wrong-helicity Dirac neutrinos (ENQVIST 1993, FULLER 1991) to set more stringent limits. DOLGOV 1996 argues that a possible window near 20 MeV is excluded.


pdgid: S066MNT
text:
SIGL 1995 exclude massive Dirac or Majorana neutrinos with lifetimes between 10**-3 and 10**8 seconds if the decay products are predominantly gamma or e+ e-.


pdgid: S066MNT
text:
DODELSON 1994 calculate constraints on nu_{{tau}} mass and lifetime from nucleosynthesis for 4 generic decay modes. Limits depend strongly on decay mode. Quoted limit is valid for all decay modes of Majorana neutrinos with lifetime greater than about 300 s. For Dirac neutrinos limits change to <0.3 or >33.


pdgid: S066MNT
text:
KAWASAKI 1994 excluded region is for Majorana neutrino with lifetime >1000 s. Other limits are given as a function of nu_{{tau}} lifetime for decays of the type nu_tau --> nu_mu phi where phi is a Nambu-Goldstone boson.


pdgid: S066MNT
text:
PERES 1994 used PDG 1992 values for parameters to obtain a value consistent with mixing. Reexamination by BOTTINO 1996 which included radiative corrections and 1995 PDG parameters resulted in two allowed regions, m(3)<70 MeV and 140 MeV m(3)<149 MeV.


pdgid: S066MNT
text:
CINABRO 1993 bound comes from analysis of tau- --> 3pi- 2pi+ nu_tau and tau- --> 2pi- pi+ 2pi0 nu_tau decay modes.


pdgid: S066MNT
text:
DOLGOV 1993 assumes neutrino lifetime >100 s. For Majorana neutrinos, the low mass limit is 0.5 MeV. KAWANO 1992 points out that these bounds can be overcome for a Dirac neutrino if it possesses a magnetic moment. See also DOLGOV 1996.


pdgid: S066MNT
text:
ALBRECHT 1992M reports measurement of a slightly lower tau mass, which has the effect of reducing the nu_{{tau}} mass reported in ALBRECHT 1988B. Bound is from analysis of tau- --> 3pi- 2pi+ nu_tau mode.


pdgid: S066MNS
text:
ABDUL-KARIM 2025 uses DESI DR2 data in combination with CMB measurements. The limit weakens to < 0.16 eV in the w_{{0}}()w_{{a}} model. This updates ADAME 2025A.


pdgid: S066MNS
text:
SHAO 2025 uses Planck CMB data with ACT lensing data, SN IA data from Pantheon+, and BAO data from SDSS and DESI. Relaxed limit assumes dynamical dark energy.


pdgid: S066MNS
text:
MADHAVACHERIL 2024 combines ACT lensing data with Planck CMB anisotropies as well as galaxy BAO and optical depth information from the SRoll2 reanalysis of the Planck data.


pdgid: S066MNS
text:
BRIEDEN 2022 combines redshift-space distortions and the shape of the matter power spectrum from BOSS and eBOSS data together with Planck CMB data. Absent the CMB data, the limit is 0.40 eV.


pdgid: S066MNS
text:
TANSERI 2022 combines BOSS galaxy clustering data with measurements of CMB data. Updates  VAGNOZZI 2017.


pdgid: S066MNS
text:
ALAM 2021 limit on the sum of neutrino masses by the eBOSS collaboration is based on galaxy, quasar, and Lyman-alpha 3D clustering data combined with Planck temperature and polarization CMB and supernovae data.


pdgid: S066MNS
text:
DI-VALENTINO 2021 combines CMB temperature and polarization, SNIa luminosity distances and baryon acoustic oscillations data.


pdgid: S066MNS
text:
GARNY 2021 employs a model for the Lyman-alpha flux power spectrum to set a limit using  BOSS data. When combined with Planck CMB temperature and polarization data, a 95% CL range  0.10 -- 0.13 eV is found.


pdgid: S066MNS
text:
STOCKER 2021 use terrestrial and cosmological experiments to set a 95% CL range on the sum of neutrino masses of 0.058 -- 0.139 eV for normal ordering and 0.098 -- 0.174 eV for inverse ordering. They also set an upper limit of 0.037 eV (NO) and 0.042 eV (IO) for the lightest neutrino mass.


pdgid: S066MNS
text:
AGHANIM 2020 limit on the sum of neutrino masses from Planck data combined with lensing and baryon acoustic oscillations (BAO). Without BAO, the limit relaxes to <0.24 eV. Several other limits are quoted based on different combinations of data.


pdgid: S066MNS
text:
CHOUDHURY 2020 combines 2018 Planck CMB temperature and polarization data plus lensing, together with baryon acoustic oscillation data from BOSS, MGS, and 6dFGS. Assumes LambdaCDM model. The upper limit is 0.17 eV for the inverted hierarchy, and 0.12 eV for degenerate neutrinos. Limits are also derived for extended cosmological models.


pdgid: S066MNS
text:
IVANOV 2020 combines 2018 Planck CMB data with baryon acoustic oscillation data from BOSS. This study is based on a full-shape likelhood for the redshift-space galaxy power spectrum of the BOSS data.


pdgid: S066MNS
text:
PALANQUE-DELABROUILLE 2020 combine Lyman alpha and Planck temperature and polarization data. Limit improves to 0.09 eV when CMB lensing and baryon acoustic oscillation data are included.


pdgid: S066MNS
text:
LOUREIRO 2019 combines data from large scale structure, cosmic microwave background, type Ia supernovae and big bang nucleosynthesis using physically motivated neutrino mass models.


pdgid: S066MNS
text:
UPADHYE 2019 uses the shape of the BOSS redshift-space galaxy power spectrum in combination with the CMB, and supernovae data. Limit weakens to < 0.54 eV if the dark energy equation of state is allowed to vary.


pdgid: S066MNS
text:
CHOUDHURY 2018 combines 2015 Planck CMB temperature data, information from the optical depth to reionization from Planck 2016 intermediate results together with baryon acoustic oscillation data from BOSS, MGS, and 6dFGS as well as supernovae Type Ia data from the Pantheon Sample. The limit is strengthened to 0.118 eV when high-l CMB polarization data is also included.


pdgid: S066MNS
text:
SIMPSON 2017 uses a combination of laboratory and cosmological measurements to determine the light neutrino masses and argue that there is strong evidence for the normal mass ordering.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos using the Lyman-alpha forest power spectrum with BOSS (mid-resolution), XQ-100 (high-resolution) and CMB. Without the CMB data, the limit relaxes to 0.8 eV. Supersedes PALANQUE-DELABROUILLE 2015A.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from Planck CMB data combined with baryon acoustic oscillation and Planck cluster data.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from BAO data from SDSS-III/BOSS combined with CMB data from Planck. Limit quoted for normal mass hierarchy. The limit for the inverted mass hierarchy is 0.20 eV and for the degenerate mass hierarchy it is 0.15 eV.


pdgid: S066MNS
text:
ROSSI 2015 sets limits on the sum of neutrino masses using BOSS Lyman alpha forest data combined with Planck CMB data and baryon acoustic oscillations.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from Planck CMB data along with WMAP polarization, high L, and BAO data.


pdgid: S066MNS
text:
Fit to the total mass of neutrinos from BOSS data along with WMAP CMB data and data from other BAO constraints and weak lensing.


pdgid: S066MNS
text:
Constraints the total mass of neutrinos (marginalizing over the effective number of neutrino species) from CMB, CMB lensing, BAO, and galaxy clustering data.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from Planck CMB data combined with baryon acoustic oscillation data from BOSS, 6dFGS, SDSS, WiggleZ data on the galaxy power spectrum, and HST data on the Hubble parameter. The limit is increased to 0.25 eV if a lower bound to the sum of neutrino masses of 0.04 eV is assumed.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from observational Hubble parameter data with seven-year WMAP data and the most recent estimate of H_{{0}}().


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from the CFHTLS combined with seven-year WMAP data and a prior on the Hubble parameter. Limit is relaxed to 0.41 eV when small scales affected by non-linearities are removed.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from the Sloan Digital Sky Survey and the five-year WMAP data.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from the 7-year WMAP data including SDSS and HST data. Limit relaxes to 1.19 eV when CMB data is used alone. Supersedes HANNESTAD 2006.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from a combination of CMB data, a recent measurement of H_{{0}}() (SHOES), and baryon acoustic oscillation data from SDSS.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from SDSS MegaZ LRG DR7 galaxy clustering data combined with CMB, HST, supernovae and baryon acoustic oscillation data. Limit relaxes to 0.47 eV when the equation of state parameter, w not= 1.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from weak lensing measurements when combined with CMB. Limit improves to 0.54 eV when supernovae and baryon acoustic oscillation observations are included. Assumes LambdaCDM model.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from five-year WMAP data. Limit improves to 0.67 eV when supernovae and baryon acoustic oscillation observations are included. Limits quoted assume the LambdaCDM model. Supersedes SPERGEL 2007.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from weak lensing measurements when combined with CMB. Limit improves to 0.03 <Sigmamass(nu)< 0.54 eV when supernovae and baryon acoustic oscillation observations are included. The slight preference for massive neutrinos at the two-sigma level disappears when systematic errors are taken into account. Assumes LambdaCDM model.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from recent Chandra X-ray observations of galaxy clusters when combined with CMB, supernovae, and baryon acoustic oscillation measurements. Assumes flat universe and constant dark-energy equation of state, w.


pdgid: S066MNS
text:
Constraints the total mass of neutrinos from recent CMB and SOSS LRG power spectrum data along with bias mass relations from SDSS, DEEP2, and Lyman-Break Galaxies. It assumes LambdaCDM model. Limit degrades to 0.59 eV in a more general wCDM model.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from neutrino oscillation experiments and cosmological data. The most conservative limit uses only WMAP three-year data, while the most stringent limit includes CMB, large-scale structure, supernova, and Lyman-alpha data.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from recent CMB, large scale structure, SN1a, and baryon acoustic oscillation data. The limit relaxes to 1.75 when WMAP data alone is used with no prior. Paper shows results with several combinations of data sets. Supersedes KRISTIANSEN 2006.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from the CMB and the large scale structure data. The most conservative limit is obtained when generic initial conditions are allowed.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from recent CMB, large scale structure, Lyman-alpha forest, and SN1a data.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from recent CMB and large scale structure data. See also GOOBAR 2006. Superseded by HANNESTAD 2010.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from the CMB experiments alone, assuming LambdaCDM Universe. FUKUGITA 2006 show that this result is unchanged by the 3-year WMAP data.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the Sloan Digital Sky Survey and the 2dF galaxy redshift survey, WMAP and 27 other CMB experiments and measurements by the HST Key project.


pdgid: S066MNS
text:
Constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the Sloan Digital Sky Survey, the 2dF galaxy redshift survey, WMAP and ACBAR. The limit is strengthened to 0.6 eV when measurements by the HST Key project and supernovae data are included.


pdgid: S066MNS
text:
Constrains the fractional contribution of neutrinos to the total matter density in the Universe from WMAP data combined with other CMB measurements, the 2dfGRS data, and Lyman alpha data. The limit does not noticeably change if the Lyman alpha data are not used.


pdgid: S066MNS
text:
LEWIS 2002 constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the CMB, HST Key project, 2dF galaxy redshift survey, supernovae type Ia, and BBN.


pdgid: S066MNS
text:
WANG 2002 constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the CMB and other cosmological data sets such as galaxy clustering and the Lyman alpha forest.


pdgid: S066MNS
text:
FUKUGITA 2000 is a limit on neutrino masses from structure formation. The constraint is based on the clustering scale sigma(8) and the COBE normalization and leads to a conservative limit of 0.9 eV assuming 3 nearly degenerate neutrinos. The quoted limit is on the sum of the light neutrino masses.


pdgid: S066MNS
text:
CROFT 1999 result based on the power spectrum of the Ly alpha forest. If Omega(matter)<0.5, the limit is improved to mass(nu)<2.4 (Omega(matter)/0.17 -- 1) eV.


pdgid: S066MSH
text:
These results apply to heavy Majorana neutrinos and are summarized by the equation: mass(nu) >1.2 GeV (G(F)/G(R)). The bound saturates, and if G(R) is too small no mass range is allowed.


pdgid: S066CHR
text:
CAPRINI 2005 limit derived from the lack of a charge asymmetry in the universe. Limit assumes that charge asymmetries between particles are not anti-correlated.


pdgid: S066CHR
text:
DEMIRCI 2025A analyzed 1540 kg.y of Xe exposure of the TPC-based PandaX-4T dark matter search. Elastic solar neutrino-electron scattering is used to derive a bound on the millicharge of neutrinos.


pdgid: S066CHR
text:
DEMIRCI 2025A analyzed 1600 kg.y of Xe exposure of the TPC-based XENONnT dark matter search. Elastic solar neutrino-electron scattering is used to derive a bound on the millicharge of neutrinos.


pdgid: S066CHR
text:
AALBERS 2023A utilize the first 60 days of data collected by the LZ dark matter search to place a limit on the electric charge of solar neutrinos. Low energy electron-recoil events are utilized. This LZ-collaboration analysis supersedes that of the external authors in ATZORI-CORONA 2023 because of a more complete treatment of experiment uncertainties.


pdgid: S066CHR
text:
ATZORI-CORONA 2023 use LUX-ZEPLIN dark matter search data published by AALBERS 2023 to place a limit on neutrino millicharge.


pdgid: S066CHR
text:
BONET 2022A use data collected by four low-threshold Ge detectors, placed 17.1 m from one of the cores of the nuclear reactors at Brokdorf to derive this limit. A spectral analysis is performed on reactor on and off data.


pdgid: S066CHR
text:
ABE 2020E obtains this result by assuming that the low-energy excess events in the XMASS detector are produced by neutrino millicharge which is common for all three neutrino flavors.


pdgid: S066CHR
text:
KHAN 2020 performed a constrained spectral fit analysis of the excess observed in the electron recoil energy spectrum by the XENON1T experiment. This range of neutrino millicharge values is one of the possible interpretations of these excess events. For the individual flavor constraints at 90% C.L. see the original reference.


pdgid: S066CHR
text:
DELLA-VALLE 2016 obtain a limit on the charge of neutrinos valid for masses of less than 10 meV. For heavier neutrinos the limit increases as a power of mass, reaching E-6 e for m = 100 meV.


pdgid: S066CHR
text:
CHEN 2014A use the Multi-Configuration RRPA method to analyze reactor nubar_{{e}} scattering on Ge atoms with 300 eV recoil energy threshold to obtain this limit.


pdgid: S066CHR
text:
STUDENIKIN 2014 uses the limit on mu_{{nu}} from BEDA 2013 and the 2.8 keV threshold of the electron recoil energy to obtain this limit.


pdgid: S066CHR
text:
GNINENKO 2007 use limit on nubar_{{e}} magnetic moment from LI 2003B to derive this result. The limit is considerably weaker than the limits on the charge of nu_{{e}} and nubar_{{e}} from various astrophysics considerations.


pdgid: S066CHR
text:
This RAFFELT 1999 limit applies to all neutrino flavors which are light enough (<5 keV) to be emitted from globular-cluster red giants.


pdgid: S066CHR
text:
This RAFFELT 1999 limit is derived from the helioseismological limit on a new energy-loss channel of the Sun, and applies to all neutrino flavors which are light enough (<1 keV) to be emitted from the sun.


pdgid: S066CHR
text:
BABU 1994 use COOPER-SARKAR 1992 limit on nu magnetic moment to derive quoted result. It applies to nu_{{tau}}.


pdgid: S066CHR
text:
DAVIDSON 1991 use data from early SLAC electron beam dump experiment to derive charge limit as a function of neutrino mass. It applies to nu_{{tau}}.


pdgid: S066CHR
text:
Exact BARBIELLINI 1987 limit depends on assumptions about the intergalactic or galactic magnetic fields and about the direct distance and time through the field. It applies to nu_{{e}}.


pdgid: S066TMR
text:
KRAKAUER 1991 quotes the limit tau/mass(nu_{{1}}) > (0.75a**2 + 21.65a + 26.3) s/eV, where a is a parameter describing the asymmetry in the neutrino decay defined as dN(gamma)/dcos(theta) = (1/2)(1 + acos(theta)) The parameter a = 0 for a Majorana neutrino, but can vary from -1 to 1 for a Dirac neutrino. The bound given by the authors is the most conservative (which applies for a = -1).


pdgid: S066TMR
text:
RAFFELT 1985 limit on the radiative decay is from solar x- and gamma-ray fluxes. Limit depends on nu flux from p p, now established from GALLEX and SAGE to be >0.5 of expectation.


pdgid: S066TMR
text:
REINES 1974 looked for nu of nonzero mass decaying radiatively to a neutral of lesser mass + gamma. Used liquid scintillator detector near fission reactor. Finds lab lifetime 6E7 s or more. Above value of (mean life)/mass assumes average effective neutrino energy of 0.2 MeV. To obtain the limit 6E7 s REINES 1974 assumed that the full nubar_{{e}} reactor flux could be responsible for yielding decays with photon energies in the interval 0.1 MeV - 0.5 MeV. This represents some overestimate so their lower limit is an over-estimate of the lab lifetime (VOGEL 1984). If so, OBERAUER 1987 may be comparable or better.


pdgid: S066TMR
text:
VALERA 2024 reports limits using IceCube data. Authors caution that the limits on nu_{{2}} and nu_{{3}} are correlated.


pdgid: S066TMR
text:
IVANEZ-BALLESTEROS 2023 reports a limit on the lifetime-to-mass ratio of the mass eigenstates nu_{{1}} and nu_{{2}} for inverted mass ordering. No limit was obtained in the case of normal mass ordering.


pdgid: S066TMR
text:
AHARMIM 2019 quotes the limit tau/mass(nu_{{2}}) for invisible nonradiative decay of nu_{{2}}. They obtained this result by analyzing the entire SNO dataset, allowing for the decay of nu_{{2}} which would cause an energy-dependent distortion of the survival probability of electron-type solar neutrinos.


pdgid: S066TMR
text:
AHARMIM 2019 quotes the limit tau/mass(nu_{{2}}) for invisible nonradiative decay of nu_{{2}}. They obtained this result by combining the tau/mass(nu_{{2}}) measurements from SNO and other solar neutrino experiments (Super-Kamiokande, KamLAND, and Borexino B8 results; Borexino and KamLAND Be7 results; the combined gallium interaction rate from GNO, GALLEX, and SAGE; and the chlorine interaction rate from Homestake). The quoted limit at 99% CL is >1.04E-3.


pdgid: S066TMR
text:
ESCUDERO 2019 sets limits on invisible neutrino decays using Planck 2018 data of tau > 1.3 -- 0.3E9 s at 95% C.L. Values in the range tau = 2 -- 16E9 s are preferred at 95% C.L. when Planck polarization data is included. Limits scale as (mass(nu)/0.05 eV)**3.


pdgid: S066TMR
text:
CECCHINI 2011 search for radiative decays of solar neutrinos into visible photons during the 2006 total solar eclipse. The range of (mean life)/mass values corresponds to a range of nu_{{1}} masses between E-4 and 0.1 eV.


pdgid: S066TMR
text:
MIRIZZI 2007 determine a limit on the neutrino radiative decay from analysis of the maximum allowed distortion of the CMB spectrum as measured by the COBE/FIRAS. For the decay nu_2 --> nu_1 the lifetime limit is ~<4E20 s for ~< 0.14 eV. For transition with the |Delta(m)(31)| mass difference the lifetime limit is ~2E19 s for ~< 0.14 eV and ~5E20 s for ~> 0.14 eV.


pdgid: S066TMR
text:
MIRIZZI 2007 determine a limit on the neutrino radiative decay from analysis of the cosmic infrared background (CIB) using the Spitzer Observatory data. For transition with the |Delta(m)(31)| mass difference they obtain the lifetime limit ~E20 s for ~<0.14 eV.


pdgid: S066TMR
text:
WONG 2007 use their limit on the neutrino magnetic moment together with the assumed experimental value of Delta(m)(13)**2~2E-3 eV**2 to obtain tau_{{13}}()/m(1)**3>3.2E27 s/eV**3 for the radiative decay in the case of the inverted mass hierarchy. Similarly to RAFFELT 1989 this limit can be violated if electric and magnetic moments are equal to each other. Analogous, but numerically somewhat different limits are obtained for tau_{{23}}() and tau_{{21}}().


pdgid: S066TMR
text:
XIN 2005 search for the gamma from radiative decay of nu_{{e}} produced by the electron capture on Cr51. No events were seen and the limit on tau/mass(nu) was derived. This is a weaker limit on the decay of nu_{{e}} than KRAKAUER 1991.


pdgid: S066TMR
text:
XIN 2005 use their limit on the neutrino magnetic moment of nu_{{e}} together with the assumed experimental value of Delta ~ 2E-3 eV**2 to obtain tau(13)/m(1)**3 > 1E23 s/eV**3 for the radiative decay in the case of the inverted mass hierarchy. Similarly to RAFFELT 1989 this limit can be violated if electric and magnetic moments are equal to each other. Analogous, but numerically somewhat different limits are obtained for tau(23) and tau(21). Again, this limit is specific for nu_{{e}}.


pdgid: S066TMR
text:
AHARMIM 2004 obtained these results from the solar nubar_{{e}} flux limit set by the SNO measurement assuming nu_{{2}} decay through nonradiative process nu_2 --> nubar_1 X, where X is a Majoron or other invisible particle. Limits are given for the cases of quasidegenerate and hierarchical neutrino masses.


pdgid: S066TMR
text:
CECCHINI 2004 obtained this bound through the observations performed on the occasion of the 21 June 2001 total solar eclipse, looking for visible photons from radiative decays of solar neutrinos. Limit is a tau/mass(nu_{{2}}) in nu_2 --> nu_1 gamma. Limit ranges from ~ 100 to 10**7 s/eV for 0.01 < mass(nu_{{1}}) < 0.1 eV.


pdgid: S066TMR
text:
EGUCHI 2004 obtained these results from the solar nubar_{{e}} flux limit set by the KamLAND measurement assuming nu_{{2}} decay through nonradiative process nu_2 --> nubar_1 X, where X is a Majoron or other invisible particle. Limits are given for the cases of quasidegenerate and hierarchical neutrino masses.


pdgid: S066TMR
text:
The ratio of the lifetime over the mass derived by BANDYOPADHYAY 2003 is for nu_{{2}}. They obtained this result using the following solar-neutrino data: total rates measured in Cl and Ga experiments, the Super-Kamiokande's zenith-angle spectra, and SNO's day and night spectra. They assumed that nu_{{1}} is the lowest mass, stable or nearly stable neutrino state and nu_{{2}} decays through nonradiative Majoron emission process, nu_2 --> nubar_1 +J, or through nonradiative process with all the final state particles being sterile. The best fit is obtained in the region of the LMA solution.


pdgid: S066TMR
text:
DERBIN 2002B (also BACK 2003B) obtained this bound for the radiative decay from the results of background measurements with Counting Test Facility (the prototype of the Borexino detector). The laboratory gamma spectrum is given as dN(gamma)/d cos(theta)= (1/2) (1 + alphacos(theta)) with alpha=0 for a Majorana neutrino, and alpha varying to -1 to 1 for a Dirac neutrino. The listed bound is for the case of alpha=0. The most conservative bound 1.5E3 s eV**-1 is obtained for the case of alpha=-1.


pdgid: S066TMR
text:
The ratio of the lifetime over the mass derived by JOSHIPURA 2002B is for nu_{{2}}. They obtained this result from the total rates measured in all solar neutrino experiments. They assumed that nu_{{1}} is the lowest mass, stable or nearly stable neutrino state and nu_{{2}} decays through nonradiative process like Majoron emission decay, nu_2 --> nu_1^' +J where nu_{{1}}^' state is sterile. The exact limit depends on the specific solution of the solar neutrino problem. The quoted limit is for the LMA solution.


pdgid: S066TMR
text:
DOLGOV 1999 places limits in the (Majorana) tau-associated nu mass-lifetime plane based on nucleosynthesis. Results would be considerably modified if neutrino oscillations exist.


pdgid: S066TMR
text:
BILLER 1998 use the observed TeV gamma-ray spectra to set limits on the mean life of any radiatively decaying neutrino between 0.05 and 1 eV. Curve shows tau(nu)/B(gamma)>0.15E21 s at 0.05 eV, >1.2E21 s at 0.17 eV, >3E21 s at 1 eV, where B(gamma) is the branching ratio to photons.


pdgid: S066TMR
text:
Limit on the radiative decay based on nonobservation of gamma's in coincidence with nu's from SN 1987A.


pdgid: S066TMR
text:
BLUDMAN 1992 sets additional limits by this method for higher mass ranges. Cosmological limits are also obtained.


pdgid: S066TMR
text:
DODELSON 1992 range is for wrong-helicity keV mass Dirac nu's from the core of neutron star in SN 1987A decaying to nu's that would have interacted in KAM2 or IMB detectors.


pdgid: S066TMR
text:
GRANEK 1991 considers heavy neutrino decays to gamma nu_L and 3nu_L, where mass(nu_{{L}})<100 keV. Lifetime is calculated as a function of heavy neutrino mass, branching ratio into gamma nu_L, and mass(nu_{{L}}).


pdgid: S066TMR
text:
KRAKAUER 1991 quotes the limit for nu_{{e}}, tau/mass(nu) > (0.3a**2 + 9.8a + 15.9) s/eV, where a is a parameter describing the asymmetry in the radiative neutrino decay defined as dN(gamma)/dcos(theta) = (1/2)(1 + acos(theta)) a = 0 for a Majorana neutrino, but can vary from -1 to 1 for a Dirac neutrino. The bound given by the authors is the most conservative (which applies for a = -1).


pdgid: S066TMR
text:
CHUPP 1989 should be multiplied by a branching ratio (about 1) and a detection efficiency (about 1/4), and pertains to radiative decay of any neutrino to a lighter or sterile neutrino.


pdgid: S066TMR
text:
RAFFELT 1989 uses KYULDJIEV 1984 to obtain taum**3 > 3E18 s eV**3 (based on nubar_e e- cross sections). The bound for the radiative decay is not valid if electric and magnetic transition moments are equal for Dirac neutrinos.


pdgid: S066TMR
text:
Model-dependent theoretical analysis of SN 1987A neutrinos. Quoted limit is for [Sum(j)|U(lepton j)|**2 Gamma(j) mass(j)]**-1, where lepton = mu, tau. Limit is 3.3E14 s/eV for lepton = e.


pdgid: S066TMR
text:
COWSIK 1977 considers variety of scenarios. For neutrinos produced in the big bang, present limits on optical photon flux require tau>10**23 s for mass(nu)~1 eV. See also COWSIK 1979 and GOLDMAN 1979.


pdgid: S066MGM
text:
APRILE 2022B use data collected with the XENONnT dark matter detector to place a limit on an enhanced magnetic moment of solar neutrinos. Supersedes APRILE 2020.


pdgid: S066MGM
text:
BEDA 2013 report nubar_e e- scattering results, using the Kalinin Nuclear Power Plant and a shielded Ge detector. The recoil electron spectrum is analyzed between 2.5 and 55 keV. Supersedes BEDA 2007. Supersedes BEDA 2010. This is the most stringent limit on the magnetic moment of reactor nubar_{{e}}.


pdgid: S066MGM
text:
AUERBACH 2001 limit is based on the LSND nu_{{e}} and nu_{{mu}} electron scattering measurements. The limit is slightly more stringent than KRAKAUER 1990.


pdgid: S066MGM
text:
ALPIZAR-VENEGAS 2025 use data collected by the CONUS+ coherent nucleus scattering experiment, conducted at 20.7 m distance to the Leibstadt nuclear power plant in Switzerland. The authors are not members of the CONUS+ collaboration and used public data to derive a limit on the magnetic moment of nubar_{{e}}.


pdgid: S066MGM
text:
DEMIRCI 2025A analyzed 1540 kg.y of Xe exposure of the TPC-based PandaX-4T dark matter search. Elastic solar neutrino-electron scattering is used to derive a bound on the magnetic moment of neutrinos.


pdgid: S066MGM
text:
DEMIRCI 2025A analyzed 1600 kg.y of Xe exposure of the TPC-based XENONnT dark matter search. Elastic solar neutrino-electron scattering is used to derive a bound on the magnetic moment of neutrinos.


pdgid: S066MGM
text:
ZENG 2025 use data of the PandaX-4T dark matter detector to derive a limit on the anomalous magnetic moment of solar neutrinos.


pdgid: S066MGM
text:
AALBERS 2023A utilize the first 60 days of data collected by the LZ dark matter search to place a limit on the magnetic moment of solar neutrinos. Low energy electron-recoil events are utilized. This LZ-collaboration analysis supersedes that of the external authors in ATZORI-CORONA 2023 because of a more complete treatment of experiment uncertainties.


pdgid: S066MGM
text:
ATZORI-CORONA 2023 use LUX-ZEPLIN dark matter search data published by AALBERS 2023 to place a limit on an enhanced magnetic moment of solar neutrinos.


pdgid: S066MGM
text:
COLOMA 2022 present a re-analysis of data taken by the COHERENT and Dresden-II experiments. The combination of both experiments is used to place a limit on the magnetic moment of electron-type neutrinos. The presented value is one-sided limit as recommended by the authors; the two-sided limit is <3.2E-10mu(B) at 90% C.L. Results based on Fef and YBe quenching models are reported in the paper. The authors are not part of either collaboration.


pdgid: S066MGM
text:
ABE 2020E observed an excess of low-energy events in the XMASS detector, which could be interpreted as a signal produced by a neutrino magnetic moment with this magnitude.


pdgid: S066MGM
text:
APRILE 2020 observed an excess of low-energy events in the XENON1T detector, which could be interpreted as a signal produced by a neutrino magnetic moment with this magnitude.


pdgid: S066MGM
text:
CAPOZZI 2020 obtains a limit on the neutrino dipole moment from the brightness of the tip of the red-giant branch in omega Centauri. A similar limit of mu_{{nu}} < 1.5E-12 mu_{{B}} is obtained in NGC 4258.


pdgid: S066MGM
text:
KHAN 2020 performed a constrained spectral fit analysis of the excess observed in the electron recoil energy spectrum by the XENON1T experiment. This range of the mu_{{B}} values is one of the possible interpretations of these excess events. For the individual flavor constraints at 90% C.L. see the original reference.


pdgid: S066MGM
text:
AGOSTINI 2017A obtained this limit using the shape of the recoil electron energy spectrum from the Borexino Phase-II 1291.5 live days of solar neutrino data and the constraints on the sum of the solar neutrino fluxes from the radiochemical gallium experiments SAGE, Gallex, and GNO. Without radiochemical constraints, the 90% C.L. limit of <4.0E-11mu(B) is obtained.


pdgid: S066MGM
text:
ARCEO-DIAZ 2015 constrains the neutrino magnetic moment from observation of the tip of the red giant branch in the globular cluster omega-Centauri.


pdgid: S066MGM
text:
MILLER-BERTOLAMI 2014B constrains the neutrino magnetic moment from observations of the white dwarf luminosity function of the Galactic disk.


pdgid: S066MGM
text:
BEDA 2010 report nubar_e e- scattering results, using the Kalinin Nuclear Power Plant  and a shielded Ge detector. The recoil electron spectrum is analyzed between 2.9 and 45 keV. Supersedes BEDA 2007. Superseded by BEDA 2013.


pdgid: S066MGM
text:
DENIZ 2010 observe reactor nubar_e e scattering with recoil kinetic energies 3 -- 8 MeV using CsI(Tl) detectors. The observed rate and spectral shape are consistent with the Standard Model prediction, leading to the reported constraint on nubar_{{e}} magnetic moment.


pdgid: S066MGM
text:
KUZNETSOV 2009 obtain a limit on the flavor averaged magnetic moment of Dirac neutrinos from the time averaged neutrino signal of SN1987A. Improves and supersedes the analysis of BARBIERI 1988 and AYALA 1999.


pdgid: S066MGM
text:
ARPESELLA 2008A obtained this limit using the shape of the recoil electron energy spectrum from the Borexino 192 live days of solar neutrino data.


pdgid: S066MGM
text:
BEDA 2007 performed search for electromagnetic nubar_{{e}}-e scattering at Kalininskaya nuclear reactor. A Ge detector with active and passive shield was used and the electron recoil spectrum between 3.0 and 61.3 keV analyzed. Superseded by BEDA 2010.


pdgid: S066MGM
text:
WONG 2007 performed search for non-standard nubar_{{e}}-e scattering at the Kuo-Sheng nuclear reactor. Ge detector equipped with active anti-Compton shield is used. Most stringent laboratory limit on magnetic moment of reactor nubar_{{e}}. Supersedes LI 2003B.


pdgid: S066MGM
text:
DARAKTCHIEVA 2005 present the final analysis of the search for non-standard nubar_{{e}}-e scattering component at Bugey nuclear reactor. Full kinematical event reconstruction of both the kinetic energy above 700 keV and scattering angle of the recoil electron, by use of TPC. Most stringent laboratory limit on magnetic moment. Supersedes DARAKTCHIEVA 2003.


pdgid: S066MGM
text:
XIN 2005 evaluated the nu_{{e}} flux at the Kuo-Sheng nuclear reactor and searched for non-standard nu_{{e}}-e scattering. Ge detector equipped with active anti-Compton shield was used. This laboratory limit on magnetic moment is considerably less stringent than the limits for reactor nubar_{{e}}, but is specific to nu_{{e}}.


pdgid: S066MGM
text:
GRIFOLS 2004 obtained this bound using the SNO data of the solar B8 neutrino flux measured with deuteron breakup. This bound applies to mu(eff) = (mu(21)**2 + mu(22)**2 + mu(23)**2)**1/2.


pdgid: S066MGM
text:
LIU 2004 obtained this limit using the shape of the recoil electron energy spectrum from the Super-Kamiokande-I 1496 days of solar neutrino data. Neutrinos are assumed to have only diagonal magnetic moments, mu_{{nu1}} = mu_{{nu2}}. This limit corresponds to the oscillation parameters in the vacuum oscillation region.


pdgid: S066MGM
text:
LIU 2004 obtained this limit using the shape of the recoil electron energy spectrum from the Super-Kamiokande-I 1496 live-day solar neutrino data, by limiting the oscillation parameter region in the LMA region allowed by solar neutrino experiments plus KamLAND. mu_{{nu1}} = mu_{{nu2}} is assumed. In the LMA region, the same limit would be obtained even if neutrinos have off-diagonal magnetic moments.


pdgid: S066MGM
text:
BACK 2003B obtained this bound from the results of background measurements with Counting Test Facility (the prototype of the Borexino detector). Standard Solar Model flux was assumed. This mu_{{nu}} can be different from the reactor mu_{{nu}} in certain oscillation scenarios (see BEACOM 1999).


pdgid: S066MGM
text:
DARAKTCHIEVA 2003 searched for non-standard nubar_{{e}}-e scattering component at Bugey nuclear reactor. Full kinematical event reconstruction by use of TPC. Superseded by DARAKTCHIEVA 2005.


pdgid: S066MGM
text:
LI 2003B used Ge detector in active shield near nuclear reactor to test for nonstandard nubar_{{e}}-e scattering.


pdgid: S066MGM
text:
GRIMUS 2002 obtain stringent bounds on all Majorana neutrino transition moments from a simultaneous fit of LMA-MSW oscillation parameters and transition moments to global solar neutrino data + reactor data. Using only solar neutrino data, a 90% CL bound of 6.3E-10mu(B) is obtained.


pdgid: S066MGM
text:
BEACOM 1999 obtain the limit using the shape, but not the absolute magnitude which is affected by oscillations, of the solar neutrino spectrum obtained by Superkamiokande (825 days). This mu(nu) can be different from the reactor mu(nu) in certain oscillation scenarios.


pdgid: S066MGM
text:
RAFFELT 1999 is an update of RAFFELT 1990. This limit applies to all neutrino flavors which are light enough (<5 keV) to be emitted from globular-cluster red giants. This limit pertains equally to electric dipole moments and magnetic transition moments, and it applies to both Dirac and Majorana neutrinos.


pdgid: S066MGM
text:
RAFFELT 1999 is essentially an update of BERNSTEIN 1963, but is derived from the helioseismological limit on a new energy-loss channel of the Sun. This limit applies to all neutrino flavors which are light enough (<1 keV) to be emitted from the Sun. This limit pertains equally to electric dipole and magnetic transition moments, and it applies to both Dirac and Majorana neutrinos.


pdgid: S066MGM
text:
ELMFORS 1997 calculate the rate of depolarization in a plasma for neutrinos with a magnetic moment and use the constraints from a big-bang nucleosynthesis on additional degrees of freedom.


pdgid: S066MGM
text:
DERBIN 1993 determine the cross section for 0.6 -- 2.0 MeV electron energy as (1.28+-0.63)xsigma(weak). However, the (reactor on -- reactor off)/(reactor off) is only ~1/100.


pdgid: S066MGM
text:
COOPER-SARKAR 1992 assume f(D_{{s}})/f(pi) = 2 and D_{{s}}, Dbar_{{s}} production cross section = 2.6 mub to calculate nu flux.


pdgid: S066MGM
text:
VIDYAKIN 1992 limit is from a e nubar_e elastic scattering experiment. No experimental details are given except for the cross section from which this limit is derived. Signal/noise was 1/10. The limit uses sin**2(theta(W)) = 0.23 as input.


pdgid: S066MGM
text:
DORENBOSCH 1991 corrects an incorrect statement in DORENBOSCH 1989 that the nu magnetic moment is < 1E-9 at the 95%CL. DORENBOSCH 1989 measures both nu_mu e and nubar e elastic scattering and assume mu(nu) = mu(nubar).


pdgid: S066MGM
text:
RAFFELT 1990 limit applies for a diagonal magnetic moment of a Dirac neutrino, or for a transition magnetic moment of a Majorana neutrino. In the latter case, the same analysis gives <1.4E-12. Limit at 95%CL obtained from deltaM(c).


pdgid: S066MGM
text:
FUKUGITA 1988 find magnetic dipole moments of any two neutrino species are bounded by mu < 10**-16 [10**-9 G/B(0)] where B(0) is the present-day intergalactic field strength.


pdgid: S066MGM
text:
For mass(nu) = 8-200 eV. NUSSINOV 1987 examines transition magnetic moments for nu_mu --> nu_e and obtain < 3E-15 for mass(nu) > 16 eV and < 6E-14 for mass(nu) > 4 eV.


pdgid: S066CRD
text:
ATZORI-CORONA 2025 reports the limit of nu_{{e}} charge radius squared by performing a global fit to nuES and CEnuNS data from BNL-E734, CCFR, CHARM-II, COHERENT, CONUS+, LAMPF, LSND, nuGEN, and TEXONO. Limits for the nu_{{mu}} and nu_{{tau}} charge radii squared are also reported.


pdgid: S066CRD
text:
DEMIRCI 2025A analyzed 1540 kg.y of Xe exposure of the TPC-based PandaX-4T dark matter search. Elastic solar neutrino-electron scattering is used to derive a bound on the square of the charge radius of neutrinos.


pdgid: S066CRD
text:
DEMIRCI 2025A analyzed 1600 kg.y of Xe exposure of the TPC-based XENONnT dark matter search. Elastic solar neutrino-electron scattering is used to derive a bound on the square of the charge radius of neutrinos.


pdgid: S066CRD
text:
CADEDDU 2018 use the data of the COHERENT experiment, AKIMOV 2018. The limit is <r(nu)**2> for nu_{{mu}} obtained from the time-dependent data. Weaker limits were obtained for charge radii of nu_{{e}} and for transition charge radii. The published value was divided by 2 to conform to the convention of this table.


pdgid: S066CRD
text:
DENIZ 2010 observe reactor nubar_e e scattering with recoil kinetic energies 3 -- 8 MeV using CsI(Tl) detectors. The observed rate and spectral shape are consistent with the Standard Model prediction, leading to the reported constraint on nubar_{{e}} charge radius.


pdgid: S066CRD
text:
Based on analysis of CCFR 98 results. Limit is on <r**2(V)> + <r**2(A)>. The CHARM II and E734 at BNL results are reanalyzed, and weaker bounds on the charge radius squared than previously published are obtained. The NuTeV result is discussed; when tentatively interpreted as nu_{{mu}} charge radius it implies <r**2(V)> + <r**2(A)> = (4.20+-1.64) x 10 **-33 cm**2.


pdgid: S066CRD
text:
Results of LEP-2 are interpreted as limits on the axial-vector charge radius squared of a Majorana nu_{{tau}}. Slightly weaker limits for both vector and axial-vector charge radius squared are obtained for the Dirac case, and somewhat weaker limits are obtained from the analysis of lower energy data (LEP-1.5 and TRISTAN).


pdgid: S066CRD
text:
AUERBACH 2001 measure nu_e e elastic scattering with LSND detector. The cross section agrees with the Standard Model expectation, including the charge and neutral current interference. The 90% CL applies to the range shown.


pdgid: S066CRD
text:
VIDYAKIN 1992 limit is from a e nubar elastic scattering experiment. No experimental details are given except for the cross section from which this limit is derived. Signal/noise was 1/10. The limit uses sin**2(theta(W)) = 0.23 as input.


pdgid: S066CRD
text:
Result is obtained from reanalysis given in ALLEN 1991, followed by our reduction to obtain 1 sigma errors.


pdgid: S007N
text:
BRIEDEN 2022 combines large scale structure data from BOSS and eBOSS including the shape of the matter power spectrum with Planck CMB data.


pdgid: S007N
text:
YEH 2022 combines Planck 2018 CMB data with BBN and observations of deuterium and Helium-4. Supersedes FIELDS 2020.


pdgid: S007N
text:
AGHANIM 2020 best fit on number of neutrino types is based on Planck data combined with lensing and baryon acoustic oscillations (BAO). Without BAO, they find 2.89+0.18-0.19. Several other values are quoted using different combinations of data.


pdgid: S007N
text:
Uses Planck Data combined with an independent standard measure of distance to the sound horizon to set a limit on the total number of neutrinos. Only CMB and early-time information are used.


pdgid: S007N
text:
ROSSI 2015 sets limits on the number of neutrino types using BOSS Lyman alpha forest data combined with Planck CMB data and baryon acoustic oscillations.


pdgid: S007N
text:
Fit to the number of neutrino degrees of freedom from Planck CMB data along with WMAP polarization, high L, and BAO data.


pdgid: S007N
text:
Fit to the number of neutrinos degrees of freedom from Planck CMB data along with BAO, shear and cluster data.


pdgid: S007N
text:
Constrains the number of neutrino degrees of freedom (marginalizing over the total mass) from CMB, CMB lensing, BAO, and galaxy clustering data.


pdgid: S007N
text:
Limit on the number of light neutrino types from observational Hubble parameter data with seven-year WMAP data, SPT, and the most recent estimate of H_{{0}}(). Best fit is 3.45+-0.65.


pdgid: S007N
text:
Limit on the number of light neutrino types from the CFHTLS combined with seven-year WMAP data and a prior on the Hubble parameter. Best fit is 4.17+1.62-1.26. Limit is relaxed to 3.98+2.02-1.20 when small scales affected by non-linearities are removed.


pdgid: S007N
text:
Constrains the number of neutrino types from recent CMB and large scale structure data. No priors on other cosmological parameters are used.


pdgid: S007N
text:
Constrains the number of neutrino types from recent CMB, large scale structure, Lyman-alpha forest, and SN1a data. The slight preference for N(nu) > 3 comes mostly from the Lyman-alpha forest data.


pdgid: S007N
text:
Constrains the number of neutrino types from recent CMB and large scale structure data. See also HAMANN 2007.


pdgid: S007N
text:
Limit on the number of neutrino types based on He4 and D/H abundance assuming a baryon density fixed to the WMAP data. Limit relaxes to 4.6 if D/H is not used or to 5.8 if only D/H and the CMB are used. See also CYBURT 2001 and CYBURT 2003.


pdgid: S007N
text:
Limit on the number of neutrino types based on combination of WMAP data and big-bang nucleosynthesis. The limit from WMAP data alone is 8.3. See also KNELLER 2001. N(nu)>=3 is assumed to compute the limit.


pdgid: S007N
text:
95% confidence level range on the number of neutrino flavors from WMAP data combined with other CMB measurements, the 2dfGRS data, and HST data.


pdgid: S076H0N
text:
ABE 2025C use the complete data set of the KamLAND-Zen experiment, corresponding to a Xe136 exposure of 2097 kg.yr. The experiment made use of 745 kg of isotopically enriched xenon. The presented result utilizes data acquired during both phases of the experiment.


pdgid: S076H0N
text:
ADAMS 2025B use 567.0 kg.yr of Te130 exposure of the CUORE high-resolution bolometric calorimeter to place a limit on this decay. CUORE operates in the LNGS laboratory.


pdgid: S076H0N
text:
AGRAWAL 2025 report a new half-life limit for the 0nubeta beta decay of Mo100, derived from 3.89 kg.yr of isotope exposure of the AMoRE-I experiment, conducted in the Yangyang Underground Laboratory in Korea.


pdgid: S076H0N
text:
ARNQUIST 2025 use the final data set collected by the MAJORANA DEMONSTRATOR experiment to place a limit on the 0nubeta beta half-life of Ge76 to one of the excited states of Se76. The data set corresponds to a Ge76 isotope exposure of 98.2 kg.yr.


pdgid: S076H0N
text:
ZHANG 2025 make use of 44.6 kg.y of Xe136 isotope exposure in the PandaX-4T TPC, using natural xenon, to place a limit on the 0nubeta beta decay half-life of Xe136.


pdgid: S076H0N
text:
YAN 2024 make use of 17.9 kg.y of Xe134 isotope exposure in the PandaX-4T TPC, using natural xenon, to place a limit on the 0nubeta beta decay half-life of Xe134.


pdgid: S076H0N
text:
ARNQUIST 2023 use the final data set of the MAJORANA DEMONSTRATOR experiment, operating enriched in Ge76 detectors, to set this limit on the 0nubeta beta half-life of Ge76. The exposure is 64.5 kg.yr. A median sensitivity of 8.1E25 yr is reported.


pdgid: S076H0N
text:
AUGIER 2023 utilize the complete data, set collected by the CUPID-Mo bolometric calorimeter  with particle ID and located at the LSM, to study various double beta  decays of Mo100 to excited states of the daughter nucleus. An exposure of 1.47  kg.yr of Mo100 is available.


pdgid: S076H0N
text:
NOVELLA 2023 use data collected by the NEXT-White experiment to limit the 0nu beta beta half-life of Xe136. The experiment contains 3.5 kg of enriched Xe and is based on a high-pressure gas TPC. Two different limits are reported, based on different data analysis approaches, > 5.5E23 yr and > 13E23 yr.


pdgid: S076H0N
text:
ADAMS 2022A use the CUORE TeO(2) experiment with an exposure of 288.8 kg.yr of Te130 to place a limit on its 0nu beta beta decay. The median sensitivity is reported as 280E23 yr. Superseeds ADAMS 2020A.


pdgid: S076H0N
text:
ADAMS 2022B use the CUORE bolometric calorimeter to place a limit on the 0nubeta beta decay half-life of Te128.


pdgid: S076H0N
text:
APRILE 2022A use 36.16 kg.yr of Xe136 exposure of the XENON1T not  enriched detector to establish the stated limit.


pdgid: S076H0N
text:
AUGIER 2022 use the final data set of the CUPID-Mo cryogenic calorimeter, utilizing enriched  Li(2)Mo100O(4) and an isotope exposure of 1.47 kg.y, to place a limit on the 0nubeta beta decay half-life.


pdgid: S076H0N
text:
AZZOLINI 2022 use the CUPID-0 scintillating cryogenic bolometer to set a limit on the 0nu beta beta half-life of Se82. The analyzed isotope exposure is 8.82 kg.yr. A median sensitivity of 7E24 yr is reported. Supersedes AZZOLINI 2019.


pdgid: S076H0N
text:
AZZOLINI 2022 use CUPID-0 data with an isotope exposure of 8.82 kg.yr to set a limit  on the 0nu beta beta decay to the first excited 0**+ state.


pdgid: S076H0N
text:
AZZOLINI 2022 use CUPID-0 data with an isotope exposure of 8.82 kg.yr to set a limit on the 0nu beta beta decay to the first excited 2**+ state.


pdgid: S076H0N
text:
AZZOLINI 2022 use CUPID-0 data with an isotope exposure of 8.82 kg.yr to set a limit on the 0nu beta beta decay to the second excited 2**+ state.


pdgid: S076H0N
text:
ADAMS 2021A et al. used 101.76 kg yr of Te130 exposure of the CUORE (LNGS)  bolometric detector to place a limit on the decay to the first excited state of Xe130,  superseding ALDUINO 2019 as the most restrictive bound on this particular decay.


pdgid: S076H0N
text:
ARMENGAUD 2021 use the CUPID-Mo 4.2 kg array of enriched Li(2)Mo100O(4)  scintillating bolometers, with 1.17 kg.yr exposure, to set this limit.


pdgid: S076H0N
text:
ARNQUIST 2021 use the MAJORANA demonstrator to set this limit for the 0nu beta beta decay to the first excited 0**+ state, with a 41.9 kg yr isotopic exposure. The median sensitivity is 39.9E23 yr.


pdgid: S076H0N
text:
ARNQUIST 2021 use the MAJORANA demonstrator to set this limit for the 0nu beta beta decay to the first excited 2**+ state, with a 41.9 kg yr isotopic exposure. The median sensitivity is 21.2E23 yr.


pdgid: S076H0N
text:
ARNQUIST 2021 use the MAJORANA demonstrator to set this limit for the 0nu beta beta decay to the second excited 2**+ state, with a 41.9 kg yr isotopic exposure. The median sensitivity is 18.6E23 yr.


pdgid: S076H0N
text:
AGOSTINI 2020B present the final data set of the GERDA experiment, searching for 0nu beta beta decay of Ge76 with isotopically enriched, high resolution Ge detectors. A final exposure of 127.2 kg.yr is reported. The experiment reports the lowest background and longest half life limit ever achieved by any double beta decay experiment. The reported experiment sensitivity equals the limit. Supersedes AGOSTINI 2019.


pdgid: S076H0N
text:
ALDUINO 2019 use the combined data of the CUORICINO and CUORE-0 experiments to place a lower limit on the half life of the 0nu beta beta decay of Te130 to the first excited 0**+ state of Xe130. Supersedes ANDREOTTI 2012.


pdgid: S076H0N
text:
ANTON 2019 uses he complete dataset of the EXO-200 detector to search for the 0nu beta beta decay. The exposure is 234.1 kg yr. The median sensitivity is 5.0E25 yr. Supersedes ALBERT 2018 and ALBERT 2014B.


pdgid: S076H0N
text:
NI 2019 use the PandaX-II dual phase TPC at CJPL to search for the 0nu beta beta decay of Xe136. The half-life limit 2.4E23 yr is obtained from 22.2 kg yr exposure with a sensitivity of 1.9E23 yr.


pdgid: S076H0N
text:
ALDUINO 2018 uses the CUORE detector to search for the 0nu beta beta decay of Te130. The exposure is 86.3 kg.year of natural TeO(2) corresponding to 24.0 kg.year for Te130. The median sensitivity is 0.7E25 yr. The limit is obtained combining the new data from CUORE with those of CUORE0 (9.8 kg.year of Te130) and Cuoricino (19.8 kg.year of Te130).


pdgid: S076H0N
text:
ARNOLD 2018 use the NEMO-3 tracking detector to place a limit on the 0 nu beta beta decay of Se82. This is a slightly weaker limit than in BARABASH 2011A, using the same detector. Supersedes ARNOLD 2005A.


pdgid: S076H0N
text:
BARABASH 2018 use 1.162 kg of Cd116WO(4) scintillating crystals to obtain this limit. Supersedes DANEVICH 2003 with analogous source and is more sensitive than ARNOLD 2017.


pdgid: S076H0N
text:
ALBERT 2017C uses the EXO-200 detector that contains 19.098+-0.014% admixture of Xe134 to search for the 0nu and 2nu beta beta decay modes. The exposure is 29.6 kg.year. The median sensitivity is 1.9E21 years.


pdgid: S076H0N
text:
ARNOLD 2017 use the NEMO-3 tracking calorimeter, containing 410 g of enriched Cd116 exposed for 5.26 yr, to determine the half-life limit. Supersedes BARABASH 2011A.


pdgid: S076H0N
text:
ALDUINO 2016 report result obtained with 9.8 kg.y of data collected with the CUORE-0 bolometer, combined with data from the CUORICINO. Supersedes ALFONSO 2015.


pdgid: S076H0N
text:
ASAKURA 2016 use the KamLAND-Zen liquid scintillator calorimeter (Xe136 89.5 kg yr) to place a limit on the 0nubetabeta-decay into the first excited state of the daughter nuclide.


pdgid: S076H0N
text:
ASAKURA 2016 use the KamLAND-Zen liquid scintillator calorimeter (Xe136 89.5 kg yr) to place a limit on the 0nubetabeta-decay into the second excited state of the daughter nuclide.


pdgid: S076H0N
text:
ASAKURA 2016 use the KamLAND-Zen liquid scintillator calorimeter (Xe136 89.5 kg yr) to place a limit on the 0nubetabeta-decay into the third excited state of the daughter nuclide.


pdgid: S076H0N
text:
ARNOLD 2015 use the NEMO-3 tracking calorimeter with 34.3 kg yr exposure to determine the  limit of 0nubetabeta-half life of Mo100. Supersedes {ARNOLD 2005A} and BARABASH 2011A.


pdgid: S076H0N
text:
ANDREOTTI 2012 use high resolution TeO(2) bolometric calorimeter to search for the 0nubetabeta decay of Te130 leading to the excited 0(+)**1 state at 1793.5 keV.


pdgid: S076H0N
text:
UMEHARA 2008 use CaF(2) scintillation calorimeter to search for double beta decay of Ca48. Limit is significantly more stringent than quoted sensitivity: 18E21 years.


pdgid: S076H0N
text:
Limit on 0nu-decay to the first excited 0(1)**+-state of daughter nucleus using NEMO-3 tracking calorimeter. Supersedes DASSIE 1995.


pdgid: S076H0N
text:
Limit on 0nu-decay to the first excited 2**+-state of daughter nucleus using NEMO-3 tracking calorimeter.


pdgid: S076H0N
text:
Supersedes ALESSANDRELLO 2000. Array of TeO(2) crystals in high resolution cryogenic calorimeter. Some enriched in Te128. Ground state to ground state decay.


pdgid: S076H0N
text:
AALSETH 2002B limit is based on 117 mol.yr of data using enriched Ge detectors. Background reduction by means of pulse shape analysis is applied to part of the data set. Reported limit is slightly less restrictive than that in KLAPDOR-KLEINGROTHAUS 2001 However, it excludes part of the allowed half-life range reported in KLAPDOR-KLEINGROTHAUS 2001B for the same nuclide. The analysis has been criticized in KLAPDOR-KLEINGROTHAUS 2004B. The criticism was addressed and disputed in AALSETH 2004.


pdgid: S076H2N
text:
ADAMS 2025A derive an improved 2nubeta beta measurement of the half-life of Te130 from 1038 kg.yr of TeO(2) exposure, with natural Te, of the CUORE experiment.


pdgid: S076H2N
text:
BARABASH 2025 use the STELLA low background Ge detectors at LNGS to search for 2nubeta beta decay of Nd150 to excited states of Sm150. The observation of 2nubeta beta decay to 0(1)**+ exited state is reported. The reported half-life value is obtained interpreting an excess observed at 334 keV as an indication of this decay.


pdgid: S076H2N
text:
BARABASH 2025A use the OBELIX Ge detector counting facility at the Laboratoire Souterrain de Modane to observe the 2nubeta beta decay of Se82 to the 0(1)**+ excited state of Kr82.


pdgid: S076H2N
text:
BO 2025A use data collected by the PandaX-4T experiment to determine the half-life of Xe124 against 2nuDEC. 1.73 ton.yr of xenon exposure were analyzed. Data-derived capture fractions are used in the analysis.


pdgid: S076H2N
text:
AALBERS 2024C report the observation of Xe124 2nuDEC. 1.39 kg.yr of isotopic exposure of the LZ dark matter experiment, collected during the first science run, were analyzed. The same capture fractions as used in APRILE 2022A were assumed.


pdgid: S076H2N
text:
AGOSTINI 2023 report an updated value for the 2nu beta beta half-life of Ge76; the final result of the GERDA Phase II experiment. A subset of the data, corresponding to an exposure of exposure is 11.8 kg.yr, is utilized. This is one of the most precise measurements of 2nu beta beta decay reported in the literature. An effective nuclear matrix element of 0.101+-0.001 is derived from this result.


pdgid: S076H2N
text:
AGUERRE 2023 report the results of a 5.25 yr search for the 2nu beta beta decay to the exited 0+ 0(1)**+ state of the daughter nucleus, using the NEMO-3 tracking calorimeter. 36.6g of Nd150 isotope were available for the measurement of this decay rate.


pdgid: S076H2N
text:
AUGIER 2023 utilize the complete data, set collected by the CUPID-Mo bolometric calorimeter  with particle ID and located at the LSM, to measure the Mo100 2 nu beta beta half-life to excited 0(1)**+ state of the daughter nucleus. An exposure of 1.47 kg.yr of Mo100 is available.


pdgid: S076H2N
text:
AUGIER 2023A use full data set collected by the CUPID-Mo experiment to derive an improved 2nu beta beta g.s. to g.s. half-life of Mo100. An exposure of 1.48 kg.yr of Mo100 is utilized. Supersedes ARMENGAUD 2020.


pdgid: S076H2N
text:
AZZOLINI 2023A report an improved measurement of the 2nu beta beta decay with an exposure of 8.82 kg.yr of Se82, collected with the CUPID-0 detector. Superseded AZZOLINI 2019B.


pdgid: S076H2N
text:
NOVELLA 2023 used the NEXT-White experiment, with a fiducial mass of 3.5 kg of enriched xenon, to measure the 2nu beta beta g.s. to g.s. half-life of Xe136. The experiment is based on a high-pressure gas TPC. Supersedes NOVELLA 2022.


pdgid: S076H2N
text:
ADAMS 2022B derive the 2nu beta beta half-life of Te128 from data of the CUORE bolometric calorimeter and the half-live ratio for Te130 / Te128 reported in BERNATOWICZ 1992.


pdgid: S076H2N
text:
APRILE 2022A report an improved Xe124 2nuDEC half-life measurement for Xe124, using data collected by the XENON1T detector with an isotopically not enriched Xe target. The analyzed Xe124 exposure is 0.87 kg.yr. The statistical significance of the signal is 7.0 sigma. The stated half-life considers captures from the K shell up to the N5 shell.This result supersedes APRILE 2019E, which exclusively considered captures from the K shell.


pdgid: S076H2N
text:
APRILE 2022B use data collected by the XENONnT dark matter experiment to derive an improved Xe124 2nuDEC half-life measurement for Xe124. This result supersedes APRILE 2022A.


pdgid: S076H2N
text:
NOVELLA 2022 report on a high-pressure gas TPC at Canfranc underground laboratory, filled with 3.5 kg (fiducial) xenon gas, used to measure the 2nu beta beta decay of Xe136. Topological track  reconstruction is utilized in the data analysis. The measurement is based on comparing runs with  isotopically enriched and depleted xenon. Other measurements with smaller error exist.


pdgid: S076H2N
text:
APRILE 2019E report first measurement of two-neutrino double electron capture in Xe124 using the XENON1T detector with a 0.73 t-yr exposure. An excess of 126+-29 events is observed at 64.3+-0.6 keV decay energy, corresponding to sqrt(Deltachi^2) = 4.4 with respect to the background-only hypothesis.


pdgid: S076H2N
text:
ARNOLD 2019 use the NEMO-3 tracking calorimeter with 34.3 kg y exposure to determine the 2nu beta beta half-life of Mo100. Supersedes ARNOLD 2015.


pdgid: S076H2N
text:
ARNOLD 2018 use the NEMO-3 tracking detector to determine the 2 nu beta beta half-life of Se82. 0.93 kg of Se82 was observed for 5.25 y. The half-life value was obtained based on the single-state-dominance (SSD) hypothesis, preferred in this case by about 2 sigma. Supersedes ARNOLD 2005A.


pdgid: S076H2N
text:
BARABASH 2018 use 1.162 kg of Cd116WO(4) scintillating crystals to obtain this value. Supersedes DANEVICH 2003 with analogous source and agrees with ARNOLD 2017 with the NEMO-3 detector.


pdgid: S076H2N
text:
ALBERT 2017C uses the EXO-200 detector that contains 19.098+-0.014% admixture of Xe134 to search for the 2nu beta beta decay mode. The exposure is 29.6 kg.year. The median sensitivity is 1.2E21 years.


pdgid: S076H2N
text:
ALDUINO 2017 use the CUORE-0 detector containing 10.8 kg of Te130 in 52 crystals of TeO(2). The exposure was 9.3 kg yr of Te130. This is a more accurate rate determination than in ARNOLD 2011 and BARABASH 2011A.


pdgid: S076H2N
text:
ARNOLD 2017 use the NEMO-3 tracking calorimeter, containing 410 grams of enriched Cd116 exposed for 5.26 years, to determine the half-life value.


pdgid: S076H2N
text:
ARNOLD 2016 use the NEMO-3 detector and a source of 6.99 g of Ca48. The half-life is based on 36.7 g year exposure. It is consistent, although somewhat longer, than the previous determinations of the half-life. Supersedes BARABASH 2011A.


pdgid: S076H2N
text:
ARNOLD 2016A use the NEMO-3 tracking calorimeter, containing 36.6 g of Nd150 exposed for 1918.5 days, to determine the half-life. Supersedes ARGYRIADES 2009.


pdgid: S076H2N
text:
AGOSTINI 2015A use 17.9 kg yr exposure of the GERDA calorimeter to derive an improved measurement of the 2nubetabeta decay half life of Ge76.


pdgid: S076H2N
text:
ARNOLD 2015 use the NEMO-3 tracking calorimeter with 34.3 kg yr exposure to determine the  2nubetabeta-half life of Mo100. Supersedes ARNOLD 2005A and ARNOLD 2004.


pdgid: S076H2N
text:
ALBERT 2014 use the EXO-200 tracking detector for a re-measurement of the 2nubetabeta-half life of Xe136. A nuclear matrix element of 0.0218+-0.0003 MeV**-1 is derived from this data. Supersedes ACKERMAN 2011.


pdgid: S076H2N
text:
GAVRILYAK 2013 use a proportional counter filled with Kr gas to search for the 2nu2K decay of Kr78. Data with the enriched and depleted Kr were used to determine signal and background. A 2.5sigma excess of events obtained with the enriched sample is interpreted as an indication for the presence of this decay.


pdgid: S076H2N
text:
GANDO 2012A use a modification of the existing KamLAND detector. The betabeta decay source/detector is 13 tons of enriched Xe136-loaded scintillator contained in an inner balloon. The 2nubetabeta decay rate is derived from the fit to the spectrum between 0.5 and 4.8 MeV. This result is in agreement with ACKERMAN 2011.


pdgid: S076H2N
text:
ARNOLD 2011 use enriched Te130 in the NEMO-3 detector to measure the 2 nu betabeta decay rate. This result is in agreement with, but more accurate than ARNABOLDI 2003.


pdgid: S076H2N
text:
ARGYRIADES 2010 use 9.4+-0.2 g of Zr96 in NEMO-3 detector and identify its 2nubetabeta decay. The result is in agreement and supersedes ARNOLD 1999.


pdgid: S076H2N
text:
BELLI 2010 use enriched Mo100 with 4 HP Ge detectors to record the 590.8 and 539.5 keV gamma rays from the decay of the 0(1)**+ state in Ru100 both in singles and coincidences. This result confirms the measurement of KIDD 2009 and ARNOLD 2007 and supersedes them.


pdgid: S076H2N
text:
First exclusive measurement of 2nu-decay to the first excited 0(1)**+-state of daughter nucleus. ARNOLD 2007 use the NEMO-3 tracking calorimeter to detect all particles emitted in decay. Result agrees with the inclusive (0nu + 2nu) measurement of DEBRAECKELEER 2001.


pdgid: S076H2N
text:
ARNOLD 2005A use the NEMO-3 tracking detector to determine the 2 nu beta beta half-life of Se82 with high statistics and low background (389 days of data taking). Supersedes ARNOLD 2004.


pdgid: S076H2N
text:
DANEVICH 2003 is calorimetric measurement of 2nubetabeta ground state decay of Cd116 using enrichedCdWO(4) scintillators. Agrees with EJIRI 1995 and ARNOLD 1996. Supersedes DANEVICH 2000.


pdgid: S076MW
text:
ABE 2025C use the complete data set of the KamLAND-Zen experiment, corresponding to a Xe136 exposure of 2097 kg.yr. The experiment made use of 745 kg of isotopically enriched xenon. The stated range of effective Majorana neutrino masses corresponds to the authors' assessment of nuclear matrix element variability.


pdgid: S076MW
text:
ADAMS 2025B use 567.0 kg.yr of Te130 exposure of the CUORE high-resolution bolometric calorimeter to place a limit on the effective Majorana neutrino mass. The range corresponds to the authors' assessment of nuclear matrix element variability.


pdgid: S076MW
text:
AGRAWAL 2025 derive a range of upper limits on the effective Majorana neutrino mass, using 3.89 kg.yr of isotope exposure of the AMoRE-I experiment. The experiment is conducted in the Yangyang Underground Laboratory in Korea. The reported range is due to the authors' evaluation of the spread of relevant nuclear matrix elements.


pdgid: S076MW
text:
ZHANG 2025 make use of 44.6 kg.y of Xe136 isotope exposure in the PandaX-4T TPC, using natural xenon, to place a limit on the 0nubeta beta decay half-life of Xe136. The derived range of effective Majorana neutrino masses reflects the author's evaluation of the spread of relevant nuclear matrix elements.


pdgid: S076MW
text:
ARNQUIST 2023 use the final data set of the MAJORANA DEMONSTRATOR experiment, with 64.5 kg.yr of isotop exposure, to derive an upper limit for <mass(beta beta)>. The range reflects the author's assessment of the variability of the theoretically calculated nuclear matrix elements.


pdgid: S076MW
text:
NOVELLA 2023 use data collected with the NEXT-White experiment to derive a range of upper limits for <mass(beta beta)>. The range reflects the author's assessment of the variability of the theoretically calculated nuclear matrix elements and both half-life limits stated in NOVELLA 2023.


pdgid: S076MW
text:
ADAMS 2022A use 1038.4 kg.yr of TeO(2) exposure collected by the CUORE experiment to determine this range of limits. The range reflects the uncertainty of nuclear matrix element calculations needed for the conversion of half-life to neutrino mass.


pdgid: S076MW
text:
APRILE 2022A use data taken with the XENON1T detector to limit the Majorana neutrino mass. 36.16 kg.yr of Xe136 exposure were utilized. The reported range of limits is due to uncertainties in the nuclear matrix elements.


pdgid: S076MW
text:
AUGIER 2022 use the final data set of the CUPID-Mo cryogenic calorimeter with an isotop exposure of 1.47 kg.y to derive a range of neutrino mass limits. The range reflects the authors' estimate of the spread of nuclear matrix element calculations.


pdgid: S076MW
text:
AZZOLINI 2022 use 8.82 kg.yr of isotopic exposure of the CPID-0 scintillating cryogenic bolometer to set this range of neutrino mass limits. The range reflects the authors' estimate of the spread of nuclear matrix element calculations.


pdgid: S076MW
text:
ARMENGAUD 2021 use the CUPID-Mo demonstrator, with 1.17 kg.yr exposure of Mo100, to set this limit. The range reflects the estimated uncertainty of the calculated nuclear matrix elements.


pdgid: S076MW
text:
AGOSTINI 2020B use the final data set of the GERDA experiment, representing an exposure of 127.2 kg.yr to derive an upper limit for <mass(beta beta)>. Isotopically enriched Ge detectors were used. The range reflects the variability of the theoretically calculated nuclear matrix elements. Supersedes AGOSTINI 2019.


pdgid: S076MW
text:
ALENKOV 2019 report the range of the effective masses <mass(beta beta)> corresponding to the 0nu beta beta decay half-life limit. It is based on the 52.1 kg.d exposure of Mo100, in the Yangyang underground laboratory. The median sensitivity is 1.1E23 years. The range of <mass(beta beta)> reflects the uncertainty of nuclear matrix elements.


pdgid: S076MW
text:
ANTON 2019 uses the complete dataset of the EXO-200 experiment to obtain these limits. The spread reflect the uncertainty in the nuclear matrix elements. Supersedes ALBERT 2018 and ALBERT 2014B.


pdgid: S076MW
text:
NI 2019 use the PandaX-II dual phase TPC at CJPL to search for the 0nu beta beta decay of Xe136 with 22.2 kg yr exposure. The range in the m(beta beta) limit of 1.3 -- 3.5 eV reflects the range of the calculated nuclear matrix elements. The sensitivity is 1.9E23 yr.


pdgid: S076MW
text:
ARNOLD 2018 use the NEMO-3 tracking detector to constrain the 0 nu beta beta decay of $^{82}$Se. The limit on <mass(beta beta)> is obtained assuming light neutrino exchange; the range reflects different calculations of the nuclear matrix elements. This is a somewhat weaker limit than in BARABASH 2011A using the same detector.


pdgid: S076MW
text:
BARABASH 2018 use 1.162 kg of Cd116WO(4) scintillating crystals to obtain these limits. The spread reflects the estimated uncertainty in the nuclear matrix element. Supersedes DANEVICH 2003.


pdgid: S076MW
text:
ARNOLD 2017 utilize NEMO-3 data, taken with enriched Cd116 to limit the effective Majorana neutrino mass. The reported range results from the use of different nuclear matrix elements. Supersedes BARABASH 2011A.


pdgid: S076MW
text:
ALDUINO 2016 place a limit on the effective Majorana neutrino mass using the combined data of the CUORE-0 and CUORICINO experiments. The range reflects the authors' evaluation of the variability of the nuclear matrix elements. Supersededs ALFONSO 2015.


pdgid: S076MW
text:
ARNOLD 2016A limit is derived from data taken with the NEMO-3 detector and Nd150. A range of nuclear matrix elements that include the effect of nuclear deformation have been used. Supersedes ARGYRIADES 2009.


pdgid: S076MW
text:
ARNOLD 2015 use the NEMO-3 tracking calorimeter with 34.3 kg yr exposure to determine the  neutrino mass limit based on the 0nubetabeta-half life of Mo100. The spread  range reflects different nuclear matrix elements. Supersedes ARNOLD 2014 and BARABASH 2011A.


pdgid: S076MW
text:
ARGYRIADES 2010 use Zr96 and the NEMO-3 tracking detector to obtain the reported mass limit. The range reflects the fluctuation of the nuclear matrix elements considered.


pdgid: S076MW
text:
Limit was obtained using CaF(2) scintillation calorimeter to search for double beta decay of Ca48. Reported range of limits reflects spread of QRPA and SM matrix element calculations used. Supersedes OGAWA 2004.


pdgid: S076MW
text:
Limit for <mass(nu)> is based on the nuclear matrix elements of STAUDT 1990 and ARNOLD 1996. Supersedes DANEVICH 2000.


pdgid: S076ETA
text:
ARNOLD 2018 use the NEMO03 tracking detector, with 0.93 kg of Se82 mass and 5.25 y exposure to obtain the limits for the hypothetical right-handed currents. Supersedes ARNOLD 2005A.


pdgid: S076ETA
text:
BARABASH 2018 use 1.162 kg of Cd116WO(4) scintillating crystals to obtain this limits for the hypothetical right-handed currents in the 0 nu beta beta decay of Cd116.


pdgid: S076ETA
text:
ARNOLD 2014 is based on 34.7 kg yr of exposure of the NEMO-3 tracking calorimeter. The reported range limit on <lambda> and <eta> reflects the nuclear matrix element uncertainty in Mo100.


pdgid: S076ETA
text:
ARNOLD 2007 use NEMO-3 half life limit for 0nu-decay of Mo100 to the first excited 2**+-state of daughter nucleus to limit the right-right handed admixture of weak currents <lambda>. This limit is not competitive when compared to the decay to the ground state.


pdgid: S076ETA
text:
Re-analysis of data originally published in KLAPDOR-KLEINGROTHAUS 2004A. Modified pulse shape analysis leads the authors to claim 6sigma statistical evidence for observation of 0nu-decay. Authors use matrix element of MUTO 1989 to determine <lambda> and <eta>. Uncertainty of nuclear matrix element is not reflected in stated errors.


pdgid: S076ETA
text:
ARNOLD 2005A derive limit for <lambda> based on Mo100 data collected with NEMO-3 detector. No limit for <eta> is given. Supersedes ARNOLD 2004.


pdgid: S076ETA
text:
ARNOLD 2005A derive limit for <lambda> based on Se82 data collected with NEMO-3 detector. No limit for <eta> is given. Supersedes ARNOLD 2004.


pdgid: S076ETA
text:
ARNOLD 2004 use the matrix elements of SUHONEN 1994 to obtain a limit for <lambda>, no limit for <eta> is given. This limit is more stringent than the limit in EJIRI 2001 for the same nucleus.


pdgid: S076ETA
text:
ARNOLD 2004 use the matrix elements of TOMODA 1991 and SUHONEN 1991 to obtain a limit for <lambda>, no limit for <eta> is given.


pdgid: S076ETA
text:
Supersedes ALESSANDRELLO 2000. Cryogenic calorimeter search. Reported a range reflecting uncertainty in nuclear matrix element calculations.


pdgid: S076ETA
text:
Limits for <lambda> and <eta> are based on nuclear matrix elements of STAUDT 1990. Supersedes DANEVICH 2000.


pdgid: S076ETA
text:
The range of the reported <lambda> and <eta> values reflects the spread of the nuclear matrix elements. On axis value assuming <mass(nu)>=0 and <lambda>=<eta>=0, respectively.


pdgid: S076ETA
text:
GUENTHER 1997 limits use the matrix elements of STAUDT 1990. Supersedes BALYSH 1995 and BALYSH 1992.


pdgid: S076ETA
text:
VUILLEUMIER 1993 uses the matrix elements of MUTO 1989. Based on a half-life limit 2.6E23 y at 90%CL.


pdgid: S076ETA
text:
BERNATOWICZ 1992 takes the measured geochemical decay width as a limit on the 0nu width, and uses the SUHONEN 1991 coefficients to obtain the least restrictive limit on eta. Further details of the experiment are given in BERNATOWICZ 1993.


pdgid: S067AER
text:
The rate of nu_{{e}} from mu decay was measured to be 0.68+-0.30 compared to the predicted flux. From K decay 1.10+-0.14 compared to the predicted flux.


pdgid: S067AER
text:
Based on the observation of 112 events when 158.1+9.2-8.6 were expected without oscillations. Including not only the number of events but also the shape of the energy distribution, the evidence for oscillation is at the level of about 4.3 sigma. Supersedes ALIU 2005.


pdgid: S067AER
text:
This ratio is based on the observation of 215 events compared to an expectation of 336+-14 without oscillations. See also ADAMSON 2008.


pdgid: S067AER
text:
This ratio is based on the observation of 107 events at the far detector 250 km away from KEK, and an expectation of 151+12-10.


pdgid: S067RER
text:
ALMAZAN 2020 use the RHF research reactor at ILL to compare their measured anti-neutrino event rate to the calculation by HUBER 2011. Reported 0.948+-0.008+-0.023+-0.023 measurement with uncertainties from statistics, systematic, and model. Note that this result is obtained for highly enriched U235 reactor fuel while most other reactor experiments utilize a low-enrichment mix of fissile nuclides.


pdgid: S067RER
text:
ADEY 2019 present a re-analysis of 1230 days of Daya Bay near detector data with reduced systematic uncertainties on the neutron detection efficiency. Note that ADEY 2019 report the measured to predicted antineutrino ratio using the reactor model of MUELLER 2011 (Huber-Mueller model). The ratio using the older ILL-Vogel model is 1.001+-0.015+-0.027.


pdgid: S067RER
text:
AN 2016 use 217 days of data (338k events) to determine the neutrino flux ratio relative to the prediction of Mueller-Huber and ILL-Vogel models (see AN 2016 for details). The reported flux ratios were corrected for theta_{{13}}() oscillation effect. The flux measurement is consistent with results from previous short-baseline reactor experiments. The measured inverse beta decay yield is 1.55+-0.04E-18 cm**2/(GW day) or sigma(f) = 5.92+-0.14E-43 cm**2/fission. About 4sigma excess of events was observed in the 4 -- 6 MeV prompt energy region.


pdgid: S067RER
text:
DENIZ 2010 observe reactor nubar_e e scattering with recoil kinetic energies 3 -- 8 MeV using CsI(Tl) detectors. The observed rate is consistent with the Standard Model prediction, leading to a constraint on sin**2(theta_{{W}}) = 0.251+-0.031(stat)+-0.024(sys).


pdgid: S067RER
text:
Updated result of KamLAND, including the data used in EGUCHI 2003. Note that the survival probabilities for different periods are not directly comparable because the effective baseline varies with power output of the reactor sources involved, and there were large variations in the reactor power production in Japan in 2003.


pdgid: S067RER
text:
EGUCHI 2003 observe reactor neutrino disappearance at ~180 km baseline to various Japanese nuclear power reactors.


pdgid: S067RER
text:
BOEHM 2001 search for neutrino oscillations at 0.75 and 0.89 km distance from the Palo Verde reactors.


pdgid: S067RER
text:
APOLLONIO 1999, APOLLONIO 1998 search for neutrino oscillations at 1.1 km fixed distance from Chooz reactors. They use nubar_e p --> e+ n in Gd-loaded scintillator target. APOLLONIO 1999 supersedes APOLLONIO 1998. See also APOLLONIO 2003 for detailed description.


pdgid: S067RER
text:
GREENWOOD 1996 search for neutrino oscillations at 18 m and 24 m from the reactor at Savannah River.


pdgid: S067RER
text:
DECLAIS 1994 result based on integral measurement of neutrons only. Result is ratio of measured cross section to that expected in standard V-A theory. Replaced by ACHKAR 1995.


pdgid: S067DU0
text:
ASHIE 2005 results are based on an exposure of 92 kton yr during the complete Super-Kamiokande I running period. The analyzed data sample consists of fully-contained single-ring e-like events with 0.1 GeV/c <p_{{e}} and mu-like events 0.2 GeV/c <p_{{mu}}, both having a visible energy < 1.33 GeV. These criteria match the definition used by FUKUDA 1994.


pdgid: S067DU0
text:
ASHIE 2005 results are based on an exposure of 92 kton yr during the complete Super-Kamiokande I running period. The analyzed data sample consists of fully-contained single-ring events with visible energy > 1.33 GeV and partially-contained events. All partially-contained events are classified as mu-like.


pdgid: S067DU0
text:
SANCHEZ 2003 result is based on an exposure of 5.9 kton yr, and updates ALLISON 1999 result. The analyzed data sample consists of fully-contained e-flavor and mu-flavor events having lepton momentum > 0.3 GeV/c.


pdgid: S067DU0
text:
FUKUDA 1996B studied neutron background in the atmospheric neutrino sample observed in the Kamiokande detector. No evidence for the background contamination was found.


pdgid: S067DU0
text:
DAUM 1995 results are based on an exposure of 2.0 kton yr which includes the data used by BERGER 1990B. This ratio is for the contained and semicontained events. DAUM 1995 also report R(mu/e) = 0.99+-0.13+-0.08 for the total neutrino induced data sample which includes upward going stopping muons and horizontal muons in addition to the contained and semicontained events.


pdgid: S067DU0
text:
FUKUDA 1994 result is based on an exposure of 7.7 kton yr and updates the HIRATA 1992 result. The analyzed data sample consists of fully-contained e-like events with 0.1<p_{{e}}<1.33 GeV/c and fully-contained mu-like events with 0.2<p_{{mu}}<1.5 GeV/c.


pdgid: S067DU0
text:
FUKUDA 1994 analyzed the data sample consisting of fully contained events with visible energy >1.33 GeV and partially contained mu-like events.


pdgid: S067DU0
text:
BECKER-SZENDY 1992B reports the fraction of nonshowering events (mostly muons from atmospheric neutrinos) as 0.36+-0.02+-0.02, as compared with expected fraction 0.51+-0.01+-0.05. After cutting the energy range to the Kamiokande limits, BEIER 1992 finds R(mu/e) very close to the Kamiokande value.


pdgid: S067DU1
text:
ADAMSON 2006 uses a measurement of 107 total neutrinos compared to an expected rate of 127+-13 without oscillations.


pdgid: S067DU1
text:
AMBROSIO 2001 result is based on the upward through-going muon tracks with E(mu)>1 GeV. The data came from three different detector configurations, but the statistics is largely dominated by the full detector run, from May 1994 to December 2000. The total live time, normalized to the full detector configuration, is 6.17 years. The first error is the statistical error, the second is the systematic error, dominated by the theoretical error in the predicted flux.


pdgid: S067DU1
text:
AMBROSIO 2000 result is based on the upgoing partially contained event sample. It came from 4.1 live years of data taking with the full detector, from April 1994 to February 1999. The average energy of atmospheric muon neutrinos corresponding to this sample is 4 GeV. The first error is statistical, the second is the systematic error, dominated by the 25% theoretical error in the rate (20% in the flux and 15% in the cross section, added in quadrature). Within statistics, the observed deficit is uniform over the zenith angle.


pdgid: S067DU1
text:
AMBROSIO 2000 result is based on the combined samples of downgoing partially contained events and upgoing stopping events. These two subsamples could not be distinguished due to the lack of timing information. The result came from 4.1 live years of data taking with the full detector, from April 1994 to February 1999. The average energy of atmospheric muon neutrinos corresponding to this sample is 4 GeV. The first error is statistical, the second is the systematic error, dominated by the 25% theoretical error in the rate (20% in the flux and 15% in the cross section, added in quadrature). Within statistics, the observed deficit is uniform over the zenith angle.


pdgid: S067DU1
text:
AMBROSIO 1998 result is for all nadir angles and updates AHLEN 1995 result. The lower cutoff on the muon energy is 1 GeV. In addition to the statistical and systematic errors, there is a Monte Carlo flux error (theoretical error) of +-0.13. With a neutrino oscillation hypothesis, the fit either to the flux or zenith distribution independently yields sin**2(2theta)=1.0 and Delta(m)**2~ a few times 10**-3 eV**2. However, the fit to the observed zenith distribution gives a maximum probability for chi**2 of only 5% for the best oscillation hypothesis.


pdgid: S067DU1
text:
CASPER 1991 correlates showering/nonshowering signature of single-ring events with parent atmospheric-neutrino flavor. They find nonshowering (~~nu_{{mu}} induced) fraction is 0.41+-0.03+-0.02, as compared with expected 0.51+-0.05 (syst).


pdgid: S067DU1
text:
AGLIETTA 1989 finds no evidence for any anomaly in the neutrino flux. They define rho = (measured number of nu_{{e}}'s)/(measured number of nu_{{mu}}'s). They report rho(measured)=rho(expected) = 0.96+0.32-0.28.


pdgid: S067DU1
text:
From this data BOLIEV 1981 obtain the limit Delta(m)**2 <= 6E-3 eV**2 for maximal mixing, nu_mu -/-> nu_mu type oscillation.


pdgid: S067DU9
text:
CLARK 1997 obtained this result by an analysis of fully contained and partially contained events in the IMB water-Cherenkov detector with visible energy >0.95 GeV.


pdgid: S067UDM
text:
ADAMSON 2012B reports the atmospheric neutrino results obtained with MINOS far detector in 2,553 live days (an exposure of 37.9 kton.yr). This result is obtained with a sample of high resolution contained-vertex muons. The quoted error is statistical only.


pdgid: S067UDM
text:
ASHIE 2005 results are based on an exposure of 92 kton yr during the complete Super-Kamiokande I running period. The analyzed data sample consists of fully-contained single-ring mu-like events with visible energy > 1.33 GeV and partially-contained events. All partially-contained events are classified as mu-like. Upward-going events are those with -1< cos(zenith angle) <-0.2 and downward-going events are those with 0.2< cos(zenith angle) <1. The mu-like up-down ratio for the multi-GeV data deviates from 1 (the expectation for no atmospheric nu_{{mu}} oscillations) by more than 12 standard deviations.


pdgid: S067UDE
text:
ASHIE 2005 results are based on an exposure of 92 kton yr during the complete Super-Kamiokande I running period. The analyzed data sample consists of fully-contained single-ring e-like events with visible energy > 1.33 GeV. Upward-going events are those with -1 < cos(zenith angle) < -0.2 and downward-going events are those with 0.2 < cos(zenith angle) < 1. The e-like up-down ratio for the multi-GeV data is consistent with 1 (the expectation for no atmospheric nu_{{e}} oscillations).


pdgid: S067MER
text:
ADAMSON 2012B reports the atmospheric neutrino results obtained with MINOS far detector in 2,553 live days (an exposure of 37.9 kton.yr). This result is obtained with a sample of high resolution contained-vertex muons. The expected ratio is calculated with no neutrino oscillation.


pdgid: S067MER
text:
ADAMSON 2006 result is obtained with the MINOS far detector with an exposure of 4.54 kton yr. The expected ratio is calculated with no neutrino oscillation.


pdgid: S067MPM
text:
ADAMSON 2012B reports the atmospheric neutrino results obtained with MINOS far detector in 2,553 live days (an exposure of 37.9 kton.yr). The muon charge ratio N(mu+)/N(mu-) represents the nubar_{{mu}}/nu_{{mu}} ratio.


pdgid: S067MPM
text:
This result is obtained with a charge-separated sample of high resolution contained-vertex muons. The quoted error is statistical only.


pdgid: S067MPM
text:
This result is obtained with a charge-separated sample of high resolution neutrino-induced rock-muons. The quoted error is statistical only.


pdgid: S067RPM
text:
ADAMSON 2012B reports the atmospheric neutrino results obtained with MINOS far detector in 2,553 live days (an exposure of 37.9 kton.yr). The muon charge ratio N(mu+)/N(mu-) represents the nubar_{{mu}}/nu_{{mu}} ratio. As far as the same oscillation parameters are used for nu and nubar, the expected nubar_{{mu}}/nu_{{mu}} ratio is almost entirely independent of any input oscillations.


pdgid: S067RPM
text:
This result is obtained with a charge-separated sample of high resolution neutrino-induced rock-muons.


pdgid: S067RPM
text:
The charge-separated samples of high resolution contained-vertex muons and neutrino-induced rock-muons are combined to obtain this result which is consistent with unity.


pdgid: S067RPM
text:
ADAMSON 2007 result is obtained with the MINOS far detector in 854.24 live days, based on neutrino-induced upward-going and horizontal muons. This result is consistent with CPT conservation.


pdgid: S067RPM
text:
ADAMSON 2006 result is obtained with the MINOS far detector with an exposure of 4.54 kton yr, based on contained events. The expected ratio is calculated by assuming the same oscillation parameters for neutrinos and antineutrinos.


pdgid: S067SNU
text:
KAETHER 2010 reports the reanalysis results of a complete GALLEX data (GALLEX I+II+III+IV, reported in HAMPEL 1999) based on the event selection with a new pulse shape analysis, which provides a better background reduction than the rise time analysis adopted in HAMPEL 1999.


pdgid: S067SNU
text:
ABDURASHITOV 2009 reports a combined analysis of 168 extractions of the SAGE solar neutrino experiment during the period January 1990 through December 2007, and updates the ABDURASHITOV 2002 result. The data are consistent with the assumption that the solar neutrino production rate is constant in time. Note that a ~15% systematic uncertainty in the overall normalization may be added to the ABDURASHITOV 2009 result, because calibration experiments for gallium solar neutrino measurements using intense Cr51 (twice by GALLEX and once by SAGE) and Ar37 (by SAGE) result in an average ratio of 0.87+-0.05 of the observed to calculated rates.


pdgid: S067SNU
text:
ALTMANN 2005 reports the complete result from the GNO solar neutrino experiment (GNO I+II+III), which is the successor project of GALLEX. Experimental technique of GNO is essentially the same as that of GALLEX. The run data cover the period 20 May 1998 through 9 April 2003.


pdgid: S067SNU
text:
HAMPEL 1999 report the combined result for GALLEX I+II+III+IV (65 runs in total), which update the HAMPEL 1996 result. The GALLEX IV result (12 runs) is 118.4+-17.8+-6.6 SNU. (HAMPEL 1999 discuss the consistency of partial results with the mean.) The GALLEX experimental program has been completed with these runs. The total run data cover the period 14 May 1991 through 23 January 1997. A total of 300 Ge71 events were observed. Note that a ~15% systematic uncertainty in the overall normalization may be added to the HAMPEL 1999 result, because calibration experiments for gallium solar neutrino measurements using intense Cr51 (twice by GALLEX and once by SAGE) and Ar37 (by SAGE) result in an average ratio of 0.87+-0.05 of the observed to calculated rates.


pdgid: S067SNU
text:
CLEVELAND 1998 is a detailed report of the Cl37 experiment at the Homestake Mine. The average solar neutrino-induced Ar37 production rate from 108 runs between 1970 and 1994 updates the DAVIS 1989 result.


pdgid: S067SES
text:
ABE 2024B reports the Super-Kamiokande-IV results for 2970 live days from September 2008 to May 2018. The electron kinetic energy threshold for most of this period was 3.49 MeV. During 53 live days of water convection studies, the electron kinetic energy threshold was 5.49 MeV. Supersedes ABE 2016C.


pdgid: S067SES
text:
ABE 2024B reports the full Super-Kamiokande I to IV results for 5805 live days. Supersedes ABE 2016C.


pdgid: S067SES
text:
ALLEGA 2024 reports this result from the nu_e e elastic scattering rate using the full data from the SNO+ detector's initial water phase. The events over the reconstructed electron kinetic energy range of 3.5 -- 15 MeV were analyzed. Supersedes ANDERSON 2019.


pdgid: S067SES
text:
AGOSTINI 2020A obtained this result from the nu_e e elastic scattering rate over the period between January 2008 and December 2016. Uses the same data as AGOSTINI 2018B, but the analysis technique is significantly improved.


pdgid: S067SES
text:
ANDERSON 2019 reports this result from the nu_e e elastic scattering rate using a 69.2 kton.day (or 114.7 days) of exposure from May through December, 2017 during the SNO+ detector's water commissioning phase. The events over the reconstructed electron kinetic energy range of 5 -- 15 MeV were analyzed. Superseded by ALLEGA 2024.


pdgid: S067SES
text:
AGOSTINI 2018B obtained this result from the nu_e e elastic scattering rate over the period between January 2008 and December 2016.


pdgid: S067SES
text:
ABE 2016C reports the combined results of the four phases of the Super-Kamiokande average flux measurements. Here the revised Super-Kamiokande-III result is used. Superseded by ABE 2024B.


pdgid: S067SES
text:
ABE 2016C reports the Super-Kamiokande-IV results for 1664 live days from September 2008 to February 2014. The analysis threshold is total electron energy of 4.0 MeV. Superseded by ABE 2024B.


pdgid: S067SES
text:
ABE 2016C revised the Super-Kamiokande-III average flux value reported in ABE 2011. Super-Kamiokande-III results are for 548 live days from August 4, 2006 to August 18, 2008. The analysis threshold is 5.0 MeV, but the event sample in the 5.0 -- 6.5 MeV total electron energy range has a total live time of 298 days. Superseded by ABE 2024B.


pdgid: S067SES
text:
ABE 2011B use a 123 kton.day exposure of the KamLAND liquid scintillation detector to measure the B8 solar neutrino flux. They utilize nu-e elastic scattering above a reconstructed-energy threshold of 5.5 MeV, corresponding to 5 MeV electron recoil energy. 299 electron recoil candidate events are reported, of which 157+-23.6 are assigned to background.


pdgid: S067SES
text:
BELLINI 2010A reports the Borexino result with 3 MeV energy threshold for scattered electrons. The data correspond to 345.3 live days with a target mass of 100 t, between July 15, 2007 and August 23, 2009.


pdgid: S067SES
text:
AHARMIM 2008 reports the results from SNO Phase III measurement using an array of He3 proportional counters to measure the rate of NC interactions in heavy water, over the period between November 27, 2004 and November 28, 2006, corresponding to 385.17 live days. A simultaneous fit was made for the number of NC events detected by the proportional counters and the numbers of NC, CC, and ES events detected by the PMTs, where the spectral distributions of the ES and CC events were not constrained to the B8 shape.


pdgid: S067SES
text:
CRAVENS 2008 reports the Super-Kamiokande-II results for 791 live days from December 2002 to October 2005. The photocathode coverage of the detector is 19% (reduced from 40% of that of Super-Kamiokande-I due to an accident in 2001). The analysis threshold for the average flux is 7 MeV.


pdgid: S067SES
text:
HOSAKA 2006 reports the final results for 1496 live days with Super-Kamiokande-I between May 31, 1996 and July 15, 2001, and replace FUKUDA 2002 results. The analysis threshold is 5 MeV except for the first 280 live days (6.5 MeV).


pdgid: S067SES
text:
AHARMIM 2005A measurements were made with dissolved NaCl (0.195% by weight) in heavy water over the period between July 26, 2001 and August 28, 2003, corresponding to 391.4 live days, and update AHMED 2004A. The CC, ES, and NC events were statistically separated. In one method, the B8 energy spectrum was not constrained. In the other method, the constraint of an undistorted B8 energy spectrum was added for comparison with AHMAD 2002 results.


pdgid: S067SES
text:
AHMAD 2002 reports the B8 solar-neutrino flux measured via nu e elastic scattering above the kinetic energy threshold of 5 MeV. The data correspond to 306.4 live days with SNO between November 2, 1999 and May 28, 2001, and updates AHMAD 2001 results.


pdgid: S067SES
text:
AHMAD 2001 reports the B8 solar-neutrino flux measured via nu e elastic scattering above the kinetic energy threshold of 6.75 MeV. The data correspond to 241 live days with SNO between November 2, 1999 and January 15, 2001.


pdgid: S067SES
text:
FUKUDA 1996 results are for a total of 2079 live days with Kamiokande II and III from January 1987 through February 1995, covering the entire solar cycle 22, with threshold E(e)>9.3 MeV (first 449 days), >7.5 MeV (middle 794 days), and >7.0 MeV (last 836 days). These results update the HIRATA 1990 result for the average B8 solar-neutrino flux and HIRATA 1991 result for the day-night variation in the B8 solar-neutrino flux. The total data sample was also analyzed for short-term variations: within experimental errors, no strong correlation of the solar-neutrino flux with the sunspot numbers was found.


pdgid: S067SCC
text:
AHMAD 2002 reports the SNO result of the B8 solar-neutrino flux measured with charged-current reaction on deuterium, nu_e d --> p p e-, above the kinetic energy threshold of 5 MeV. The data correspond to 306.4 live days with SNO between November 2, 1999 and May 28, 2001, and updates AHMAD 2001 results. The complete description of the SNO Phase I data set is given in AHARMIM 2007.


pdgid: S067SCC
text:
AHMAD 2001 reports the first SNO result of the B8 solar-neutrino flux measured with the charged-current reaction on deuterium, nu_e d --> p p e-, above the kinetic energy threshold of 6.75 MeV. The data correspond to 241 live days with SNO between November 2, 1999 and January 15, 2001.


pdgid: S067SNC
text:
APRILE 2024A reports measurements of B8 solar neutrinos through coherent scattering with xenon nuclei based on an exposure of 3.51 ton.yr with the XENONnT experiment.


pdgid: S067SNC
text:
BO 2024 reports measurements of B8 solar neutrinos through coherent scattering with xenon nuclei in the commissioning run and the first science run of the PandaX-4T experiment. Supersedes MA 2023A.


pdgid: S067SNC
text:
MA 2023A searched for B8 solar neutrinos elastically scattered off xenon nuclei in the commissioning phase of the PANDAX-4T experiment with an effective exposure of 0.48 ton.yr. This experiment is dedicated to dark matter direct search using a dual-phase xenon  TPC with a sensitive volume of 3.7 tons of liquid Xe. Superseded by BO 2024.


pdgid: S067SNC
text:
AHARMIM 2013 obtained this result from a combined analysis of the data from all three phases, SNO-I, II, and III. The measurement of the B8 flux mostly comes from the NC signal, however, CC contribution is included in the fit.


pdgid: S067SNC
text:
AHARMIM 2010 reports this result from a joint analysis of SNO Phase I+II data with the "effective electron kinetic energy" threshold of 3.5 MeV. This result is obtained with a "binned-histogram unconstrained fit" where binned probability distribution functions of the neutrino signal observables were used without any model constraints on the shape of the neutrino spectrum.


pdgid: S067SNC
text:
AHMAD 2002 reports the first SNO result of the B8 solar-neutrino flux measured with the neutral-current reaction on deuterium, nu_lepton d --> n p nu_lepton, above the neutral-current reaction threshold of 2.2 MeV. The data correspond to 306.4 live days with SNO between November 2, 1999 and May 28, 2001. The complete description of the SNO Phase I data set is given in AHARMIM 2007.


pdgid: S067SB8
text:
AHMAD 2002 deduced the nonelectron-flavor active neutrino component (nu_{{mu}} and nu_{{tau}}) in the B8 solar-neutrino flux, by combining the charged-current result, the nu e elastic-scattering result and the neutral-current result. The complete description of the SNO Phase I data set is given in AHARMIM 2007.


pdgid: S067SB8
text:
AHMAD 2001 deduced the nonelectron-flavor active neutrino component (nu_{{mu}} and nu_{{tau}}) in the B8 solar-neutrino flux, by combining the SNO charged-current result (AHMAD 2001) and the Super-Kamiokande nu e elastic-scattering result (FUKUDA 2001).


pdgid: S067PPT
text:
AGOSTINI 2018B obtained this result from the measured nu_e e elastic scattering rate over the period between December 2011 and May 2016, assuming the MSW-LMA oscillation parameters derived by ESTEBAN 2017. Assuming a high-metalicity standard solar model, the electron neutrino survival probability for the p p solar neutrino is calculated to be 0.57+-0.09.


pdgid: S067B7T
text:
AGOSTINI 2018B obtained this result from the measured nu_e e elastic scattering rate over the period between December 2011 and May 2016, assuming the MSW-LMA oscillation parameters derived by ESTEBAN 2017. Assuming a high-metalicity standard solar model, the electron neutrino survival probability for the Be7 solar neutrino is calculated to be 0.53+-0.05.


pdgid: S067PET
text:
AGOSTINI 2018B obtained this result from the measured nu_e e elastic scattering rate over the period between December 2011 and May 2016, assuming the MSW-LMA oscillation parameters derived by ESTEBAN 2017 and a high-metalicity standard solar model. The electron neutrino survival probability for the pep solar neutrino is calculated to be 0.43+-0.11.


pdgid: S067SBT
text:
ANDERSON 2019 reports this result from the measured nu_e e elastic scattering rate using a 69.2 kton.day (or 114.7 days) of exposure from May through December, 2017 during the SNO+ detector's water commissioning phase, assuming the neutrino mixing parameters given in PDG 2016 and a standard solar model given in BAHCALL 2005.


pdgid: S067SBT
text:
AGOSTINI 2018B obtained this result from the measured nu_e e elastic scattering rate over the period between January 2008 and December 2016, assuming the MSW-LMA oscillation parameters derived by ESTEBAN 2017. Assuming a high-metalicity standard solar model, the electron neutrino survival probability for the B8 solar neutrino is calculated to be 0.37+-0.08.


pdgid: S067SBT
text:
AHARMIM 2010 reports this result from a joint analysis of SNO Phase I+II data with the "effective electron kinetic energy" threshold of 3.5 MeV. This result is obtained with the assumption of unitarity, which relates the NC, CC, and ES rates. The data were fit with the free parameters directly describing the total B8 neutrino flux and the energy-dependent nu_{{e}} survival probability.


pdgid: S067SBT
text:
AHMAD 2002 determined the total flux of active B8 solar neutrinos by directly measuring the neutral-current reaction, nu_lepton d --> n p nu_lepton, which is equally sensitive to nu_{{e}}, nu_{{mu}}, and nu_{{tau}}. The complete description of the SNO Phase I data set is given in AHARMIM 2007.


pdgid: S067SBT
text:
AHMAD 2001 deduced the total flux of active B8 solar neutrinos by combining the SNO charged-current result (AHMAD 2001) and the Super-Kamiokande nu e elastic-scattering result (FUKUDA 2001).


pdgid: S067CNT
text:
BASILICO 2023 obtained this result by combining the newly developed Correlated Integrated Directionality (CID)-based CNO result obtained by using the complete Borexino data-taking period from 2007 to 2021, with a spectral fit of the Phase-III dataset (from July 2016 to October 2021, characterized by a thermally stable detector). Note that the directional information is independent from the spectral information on which the previous CNO solar neutrino measurements by Borexino were based. Neutrino flavor conversion was taken into account.


pdgid: S067CNT
text:
APPEL 2022 obtained this result from the measured nu_e e elastic scattering rate over the period between January 2017 and October 2021, assuming the MSW-LMA oscillation parameters derived by ESTEBAN 2020A. The exposure corresponding to this data is 1431.6 days x 71.3 tons.


pdgid: S067CNT
text:
AGOSTINI 2020D obtained this result from the measured nu_e e elastic scattering rate over the period between July 2016 to February 2020, assuming the MSW-LMA oscillation parameters derived by CAPOZZI 2018.


pdgid: S067CNT
text:
AGOSTINI 2018B obtained this result from an upper limit of the nu_e e elastic scattering rate for the CNO neutrinos over the period between December 2011 and May 2016, assuming the MSW-LMA oscillation parameters derived by ESTEBAN 2017.


pdgid: S067HPT
text:
AGOSTINI 2020A obtained this result from an upper limit of the nu_e e elastic scattering rate and NC-mediated inelastic scattering on carbon nuclei with 15.1 MeV deexcitation gamma-ray for the hep neutrino. The dataset corresponds to an effective exposure of 0.745 kt.yr from November 2009 to October 2017. A FADC DAQ system, optimized for the acquisition of high-energy events was used for data collection. The MSW-LMA oscillation parameters derived by ESTEBAN 2017 were assumed.


pdgid: S067HPT
text:
AHARMIM 2020 uses the entire SNO dataset, corresponding to 2.47 kton.yrs of exposure after fiducialization. With the D(2)O target, SNO was sensitive to charged current, neutral current, and elastic scattering channels.


pdgid: S067HPT
text:
AGOSTINI 2018B obtained this result from an upper limit of the nu_e e elastic scattering rate for the hep neutrino using the dataset corresponding to an exposure of 0.8 kt.yr and assuming the MSW-LMA oscillation parameters derived by ESTEBAN 2017.


pdgid: S067SDN
text:
ABE 2024B reports the combined day-night flux asymmetry results of the four phases (5805 live days) of the Super-Kamiokande measurements. Amplitude fit method is used. Supersedes ABE 2016C.


pdgid: S067SDN
text:
ABE 2024B reports the day-night flux asymmetry of the Super-Kamiokande IV data (2970 live days). Amplitude fit method is used. Supersedes ABE 2016C.


pdgid: S067SDN
text:
ABE 2016C reports the combined day-night flux asymmetry results of the four phases of the Super-Kamiokande measurements. Amplitude fit method is used. See footnote to RENSHAW 2014. Superseded by ABE 2024B.


pdgid: S067SDN
text:
ABE 2016C reports the Super-Kamiokande-IV results for 1664 live days from September 2008 to February 2014. The analysis threshold for day-night flux asymmetry is recoil electron energy of 4.49 MeV (total electron energy of 5.0 MeV). Amplitude fit method is used. See footnote to RENSHAW 2014. Superseded by ABE 2024B.


pdgid: S067SDN
text:
RENSHAW 2014 obtains this result by using the "amplitude fit" introduced in SMY 2004. The data from the Super-Kamiokande(SK)-I, -II, -III, and 1306 live days of the SK-IV measurements are used. The analysis threshold is recoil-electron kinetic energy of 4.5 MeV for SK-III, and SK-IV except for 250 live days in SK-III (6.0 MeV). The analysis threshold for SK-I and SK-II is the same as in the previous reports. (Note that in the previous SK solar-neutrino results, the analysis threshold is quoted as recoil-electron total energy.) This day-night asymmetry result is consistent with neutrino oscillations for 4E-5 eV**2 < Deltam(21)**2 < 7E-5 eV**2 and large mixing values of theta(12) at the 68% CL.


pdgid: S067SDN
text:
CRAVENS 2008 reports the Super-Kamiokande-II results for 791 live days from December 2002 to October 2005. The photocathode coverage of the detector is 19% (reduced from 40% of that of Super-Kamiokande-I due to an accident in 2001). The analysis threshold for the day and night fluxes is 7.5 MeV except for the first 159 live days (8.0 MeV).


pdgid: S067SDN
text:
This result with reduced statistical uncertainty is obtained by assuming two-neutrino oscillations within the LMA (large mixing angle) region and by fitting the time variation of the solar neutrino flux measured via nu_{{e}}() elastic scattering to the variations expected from neutrino oscillations. For details, see SMY 2004. There is an additional small systematic error of +-0.0004 coming from uncertainty of oscillation parameters.


pdgid: S067SDN
text:
AHARMIM 2005A measurements were made with dissolved NaCl (0.195% by weight) in heavy water over the period between July 26, 2001 and August 28, 2003, with 176.5 days of the live time recorded during the day and 214.9 days during the night. This result is obtained with the spectral distribution of the CC events not constrained to the B8 shape.


pdgid: S067SDN
text:
AHMAD 2002B results are based on the charged-current interactions recorded between November 2, 1999 and May 28, 2001, with the day and night live times of 128.5 and 177.9 days, respectively. The complete description of the SNO Phase I data set is given in AHARMIM 2007.


pdgid: S067SDN
text:
AHMAD 2002B results are derived from the charged-current interactions, neutral-current interactions, and nu e elastic scattering, with the total flux of active neutrinos constrained to have no asymmetry. The data were recorded between November 2, 1999 and May 28, 2001, with the day and night live times of 128.5 and 177.9 days, respectively. The complete description of the SNO Phase I data set is given in AHARMIM 2007.


pdgid: S067PBE
text:
GANDO 2015 uses 165.4 kton.day exposure of the KamLAND liquid scintillator detector to measure the 862 keV Be7 solar neutrino flux via nu-e elastic scattering


pdgid: S067PBE
text:
BELLINI 2011A reports the Be7 solar neutrino flux measured via nu-e elastic scattering. The data correspond to 740.7 live days between May 16, 2007 and May 8, 2010, and also correspond to 153.6 ton.year fiducial exposure. BELLINI 2011A measured the 862 keV Be7 solar neutrino flux, which is an 89.6% branch of the Be7 solar neutrino flux, to be 2.78+-0.13E9 cm**-2 s**-1. Supercedes ARPESELLA 2008A.


pdgid: S067PEP
text:
BELLINI 2012A reports 1.44 MeV p e p solar-neutrino flux measured via nu_{{e}} elastic scattering. The data were collected between January 13, 2008 and May 9, 2010, corresponding to 20,4009 ton.day fiducial exposure. The listed flux value is calculated from the observed rate of p e p solar neutrino interactions in Borexino (3.1+-0.6+-0.3 counts/(day.100 ton)) and the corresponding rate expected for no neutrino flavor oscillations (4.47+-0.05 counts/(day.100 ton)), using the SSM prediction for the p e p solar neutrino flux of 1.441+-0.012E8 cm**-2s**-1.


pdgid: S067CNO
text:
BELLINI 2012A reports an upper limit of the CNO solar neutrino flux measured via nu_{{e}} elastic scattering. The data were collected between January 13, 2008 and May 9, 2010, corresponding to 20,409 ton.day fiducial exposure.


pdgid: S067PPC
text:
LU 2024 searched for p p solar neutrinos via nu e elastic scattering using PandaX-4T commissioning data. By fitting the measured energy spectrum of events in the 24 -- 144 keV recoil electron kinetic energy, the number of p p + Be7 neutrinos is measured to be 231+-113+-287 events. The p p neutrino flux is estimated using the expected ratio of p p to Be7 fluxes and their contributions to the measured energy range.


pdgid: S067PPC
text:
BELLINI 2014A reports p p solar-neutrino flux measured via nu e elastic scattering. The data were collected between January 2012 and May 2013, corresponding to 408 days of data. The p p neutrino interaction rate in Borexino is measured to be 144+-13+-10 counts/(day.100 ton) by fitting the measured energy spectrum of events in the 165 -- 590 keV recoil electron kinetic energy window with the expected signal + background spectrum. The listed flux value phi_{{ES}}(p p) is calculated from the observed rate and the number of 3.307+-0.003E31 electrons for 100 tons of the Borexino scintillator, and the nu_e e integrated cross section over the p p neutrino spectrum, CS(nu_e e) = 11.38E-46 cm**2.


pdgid: S067PPF
text:
ABDURASHITOV 2009 reports the p p solar-neutrino flux derived from the Ga solar neutrino capture rate by subtracting contributions from B8, Be7, p e p and CNO solar neutrino fluxes determined by other solar neutrino experiments as well as neutrino oscillation parameters determined from available world neutrino oscillation data.


pdgid: S067HEP
text:
HOSAKA 2006 result is obtained from the recoil electron energy window of 18 -- 21 MeV, and updates FUKUDA 2001 result.


pdgid: S067EB8
text:
AGOSTINI 2021 derived this result relative to the Standard Solar Model B8 solar   neutrino flux, under an assumption of high solar metallicity, of 5.46 (1+-0.12)xE6  cm**-2s**-1 (see VINYOLES 2017).


pdgid: S067EB8
text:
BALATA 2006 obtained this result from the search for nubar_{{e}} interactions with Counting Test Facility  (the prototype of the Borexino detector).


pdgid: S067P12
text:
ABE 2024B obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0218+-0.0007 coming from reactor neutrino experiments, using all solar and KamLAND data. The result includes the full Super-Kamiokande I to IV data. CPT invariance is assumed. Supersedes ABE 2016C.


pdgid: S067P12
text:
ABREU 2025A report reactor anti-neutrino disappearance, observed using 286 ton.yr of data collected by the SNO+ experiment. The result is based on an extended log likelihood fit to unbinned data performed on the prompt energy distribution.


pdgid: S067P12
text:
ABREU 2025A combine results from a spectral fit to 286 ton.yr of SNO+ with KamLAND and all solar data, as reported in ABE 2016C, to obtain an improved measurement of the mixing angle. CPT invariance is assumed.


pdgid: S067P12
text:
ABE 2024B obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0218+-0.0007 coming from reactor neutrino experiments, using all solar data. CPT invariance is assumed. Supersedes ABE 2016C.


pdgid: S067P12
text:
ABE 2024B obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0218+-0.0007 coming from reactor neutrino experiments and a constraint on B8(hep) flux based on the SNO neutral current event rate, using full Super-Kamiokande (I+II+III+IV) data. CPT invariance is assumed. Supersedes ABE 2016C.


pdgid: S067P12
text:
SALAS 2021 reports results of a global fit to neutrino oscillation data available at the time of the Neutrino 2020 conference.


pdgid: S067P12
text:
ESTEBAN 2020A reports results of a global fit to neutrino oscillation data available at the time of the Neutrino2020 conference.


pdgid: S067P12
text:
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0219+-0.0014 coming from reactor neutrino experiments, using all solar data and KamLAND data. CPT invariance is assumed. Superseded by ABE 2024B.


pdgid: S067P12
text:
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0219+-0.0014 coming from reactor neutrino experiments, using Super-Kamiokande (I+II+III+IV) and SNO data. Superseded by ABE 2024B.


pdgid: S067P12
text:
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0219+-0.0014 coming from reactor neutrino experiments, by combining the four phases of the Super-Kamiokande solar data. Superseded by ABE 2024B.


pdgid: S067P12
text:
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0219+-0.0014 coming from reactor neutrino experiments, using the Super-Kamiokande-IV data. Superseded by ABE 2024B.


pdgid: S067P12
text:
FORERO 2014 performs a global fit to neutrino oscillations using solar, reactor, long-baseline accelerator, and atmospheric neutrino data.


pdgid: S067P12
text:
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as 0.304+0.013-0.012 for normal and 0.305+0.012-0.013 for inverted mass ordering.


pdgid: S067P12
text:
AHARMIM 2013 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data.


pdgid: S067P12
text:
AHARMIM 2013 global solar neutrino data include SNO's all-phases-combined analysis results on the total active B8 neutrino flux and energy-dependent nu_{{e}} survival probability parameters, measurements of Cl (CLEVELAND 1998), Ga (ABDURASHITOV 2009 which contains combined analysis with GNO (ALTMANN 2005 and Ph.D. thesis of F. Kaether)), and Be7 (BELLINI 2011A) rates, and B8 solar-neutrino recoil electron measurements of SK-I (HOSAKA 2006) zenith, SK-II (CRAVENS 2008) and SK-III (ABE 2011) day/night spectra, and Borexino (BELLINI 2010A) spectra.


pdgid: S067P12
text:
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(32) fixed to 2.45E-3 eV**2, using global solar neutrino data.


pdgid: S067P12
text:
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(32) fixed to 2.45E-3 eV**2, using global solar neutrino and KamLAND (GANDO 2011) data. CPT invariance is assumed.


pdgid: S067P12
text:
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND, global solar neutrino, short-baseline (SBL) reactor, and accelerator data, assuming CPT invariance. Supersedes GANDO 2011.


pdgid: S067P12
text:
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND and global solar neutrino data, assuming CPT invariance. Supersedes GANDO 2011.


pdgid: S067P12
text:
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND data. Supersedes GANDO 2011.


pdgid: S067P12
text:
ABE 2011 obtained this result by a two-neutrino oscillation analysis using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, SAGE, and KamLAND data. CPT invariance is assumed.


pdgid: S067P12
text:
ABE 2011 obtained this result by a two-neutrino oscillation analysis using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, and SAGE data.


pdgid: S067P12
text:
ABE 2011 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(32) fixed to 2.4E-3 eV**2, using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, SAGE, and KamLAND data. The normal neutrino mass ordering and CPT invariance are assumed.


pdgid: S067P12
text:
ABE 2011 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(32) fixed to 2.4E-3 eV**2, using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, and GALLEX/GNO data. The normal neutrino mass ordering is assumed.


pdgid: S067P12
text:
BELLINI 2011A obtained this result by a two-neutrino oscillation analysis using KamLAND, Homestake, SAGE, Gallex, GNO, Kamiokande, Super-Kamiokande, SNO, and Borexino (BELLINI 2011A) data and the SSM flux prediction in SERENELLI 2011 (Astrophysical Journal 743 24 (2011)) with the exception that the B8 flux was left free. CPT invariance is assumed.


pdgid: S067P12
text:
BELLINI 2011A obtained this result by a two-neutrino oscillation analysis using Homestake, SAGE, Gallex, GNO, Kamiokande, Super-Kamiokande, SNO, and Borexino (BELLINI 2011A) data and the SSM flux prediction in SERENELLI 2011 (Astrophysical Journal 743 24 (2011)) with the exception that the B8 flux was left free.


pdgid: S067P12
text:
GANDO 2011 obtain this result with three-neutrino fit using the KamLAND + solar data. Superseded by GANDO 2013.


pdgid: S067P12
text:
GANDO 2011 obtain this result with three-neutrino fit using the KamLAND data only. Superseded by GANDO 2013.


pdgid: S067P12
text:
AHARMIM 2010 global solar neutrino data include SNO's low-energy-threshold analysis survival probability day/night curves, SNO Phase III integral rates (AHARMIM 2008), Cl (CLEVELAND 1998), SAGE (ABDURASHITOV 2009), Gallex/GNO (HAMPEL 1999, ALTMANN 2005), Borexino (ARPESELLA 2008A), SK-I zenith (HOSAKA 2006), and SK-II day/night spectra (CRAVENS 2008).


pdgid: S067P12
text:
AHARMIM 2010 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data and KamLAND data (ABE 2008A). CPT invariance is assumed.


pdgid: S067P12
text:
AHARMIM 2010 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data.


pdgid: S067P12
text:
AHARMIM 2010 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(31) fixed to 2.3E-3 eV**2, using global solar neutrino data and KamLAND data (ABE 2008A). CPT invariance is assumed.


pdgid: S067P12
text:
AHARMIM 2010 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(31) fixed to 2.3E-3 eV**2, using global solar neutrino data.


pdgid: S067P12
text:
ABE 2008A obtained this result by a rate + shape + time combined geoneutrino and reactor two-neutrino fit for Deltamass**2(21) and tan**2(theta)(12), using KamLAND data only. Superseded by GANDO 2011.


pdgid: S067P12
text:
ABE 2008A obtained this result by means of a two-neutrino fit using KamLAND, Homestake, SAGE, GALLEX, GNO, SK (zenith angle and E-spectrum), the SNO chi**2-map, and solar flux data. CPT invariance is assumed. Superseded by GANDO 2011.


pdgid: S067P12
text:
The result given by AHARMIM 2008 is theta = (34.4+1.3-1.2)degrees. This result is obtained by a two-neutrino oscillation analysis using solar neutrino data including those of Borexino (ARPESELLA 2008A) and Super-Kamiokande-I (HOSAKA 2006), and KamLAND data (ABE 2008A). CPT invariance is assumed.


pdgid: S067P12
text:
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using SK nu_{{e}} data, CC data from other solar neutrino experiments, and KamLAND data (ARAKI 2005). CPT invariance is assumed.


pdgid: S067P12
text:
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using the data from Super-Kamiokande, SNO (AHMAD 2002 and AHMAD 2002B), and KamLAND (ARAKI 2005) experiments. CPT invariance is assumed.


pdgid: S067P12
text:
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using the Super-Kamiokande and SNO (AHMAD 2002 and AHMAD 2002B) solar neutrino data.


pdgid: S067P12
text:
The result given by AHARMIM 2005A is theta = (33.9+-1.6)degrees. This result is obtained by a two-neutrino oscillation analysis using SNO pure deuteron and salt phase data, SK nu_{{e}} data, Cl and Ga CC data, and KamLAND data (ARAKI 2005). CPT invariance is assumed. AHARMIM 2005A also quotes theta = (33.9+2.4-2.2)degrees as the error enveloping the 68% CL two-dimensional region. This translates into sin**2(2 theta) = 0.86+0.05-0.06.


pdgid: S067P12
text:
AHARMIM 2005A obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95% CL two-dimensional region shown in figure 35a of AHARMIM 2005A. AHARMIM 2005A also quotes tan**2(theta) = 0.45+0.09-0.08 as the error enveloping the 68% CL two-dimensional region. This translates into sin**2(2 theta) = 0.86+0.05-0.07.


pdgid: S067P12
text:
ARAKI 2005 obtained this result by a two-neutrino oscillation analysis using KamLAND and solar neutrino data. CPT invariance is assumed. The 1sigma error shown here is translated from the number provided by the KamLAND collaboration, tan**2(theta) = 0.40+0.07-0.05. The corresponding number quoted in ARAKI 2005 is tan**2(theta) = 0.40+0.10-0.07 (sin**2(2 theta) = 0.82+-0.07), which envelops the 68% CL two-dimensional region.


pdgid: S067P12
text:
The result given by AHMED 2004A is theta = (32.5+1.7-1.6)degrees. This result is obtained by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (EGUCHI 2003). CPT invariance is assumed. AHMED 2004A also quotes theta = (32.5+2.4-2.3)degrees as the error enveloping the 68% CL two-dimensional region. This translates into sin**2(2 theta) = 0.82+-0.06.


pdgid: S067P12
text:
AHMED 2004A obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95% CL two-dimensional region shown in Fig. 5(a) of AHMED 2004A. The best-fit point is Delta(m)**2 = 6.5E-5 eV**2, tan**2(theta) = 0.40 (sin**2(2 theta) = 0.82).


pdgid: S067P12
text:
The result given by SMY 2004 is tan**2(theta) = 0.44+-0.08. This result is obtained by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (IANNI 2003). CPT invariance is assumed.


pdgid: S067P12
text:
SMY 2004 obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The 1sigma errors are read from Fig. 6(a) of SMY 2004.


pdgid: S067P12
text:
SMY 2004 obtained this result by a two-neutrino oscillation analysis using the Super-Kamiokande and SNO (AHMAD 2002 and AHMAD 2002B) solar neutrino data. The 1sigma errors are read from Fig. 6(a) of SMY 2004.


pdgid: S067P12
text:
AHMAD 2002B obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95% CL two-dimensional region shown in Fig. 4(b) of AHMAD 2002B. The best fit point is Delta(m)**2 = 5.0E-5 eV**2 and tan(theta) = 0.34 (sin**2(2 theta) = 0.76).


pdgid: S067P12
text:
FUKUDA 2002 obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95% CL two-dimensional region shown in Fig. 4 of FUKUDA 2002. The best fit point is Delta(m)**2 = 6.9E-5 eV**2 and tan**2(theta) = 0.38 (sin**2(2 theta) = 0.80).


pdgid: S067DM3
text:
ABREU 2025A report the observation of reactor anti-neutrino disappearance, using 286 ton.yr of data collected by the SNO+ experiment. The result is based on an extended log likelihood fit to unbinned data performed on the prompt energy distribution.


pdgid: S067DM3
text:
ALLEGA 2025 use the reactor anti-neutrino signal collected during 125.4 days of data taking with the partially liquid scintillator filled SNO+ detector to determine Deltam(21)**2 by means of a spectral fit. Because of the low signal strength of 9.53+-0.30 inverse beta decay events, sin**2(theta_{{12}}) was fixed to the value given in PDG 2020.


pdgid: S067DM3
text:
ABREU 2025A combine results from a spectral fit to 286 ton.yr of SNO+ with KamLAND and all solar data, as reported in ABE 2016C, to obtain an improved measurement of the mass difference. CPT invariance is assumed.


pdgid: S067DM3
text:
ABE 2024B obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0218+-0.0007 coming from reactor neutrino experiments and a constraint on B8(hep) flux based on the SNO neutral current event rate, using the full Super-Kamiokande I to IV data. Supersedes ABE 2016C.


pdgid: S067DM3
text:
ABE 2024B obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0218+-0.0007 coming from reactor neutrino experiments, using SNO and full Super-Kamiokande I to IV data. Supersedes ABE 2016C.


pdgid: S067DM3
text:
ABE 2024B obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0218+-0.0007 coming from reactor neutrino experiments and a constraint on B8(hep) flux based on the SNO neutral current event rate, using the full Super-Kamiokande IV data. Supersedes ABE 2016C.


pdgid: S067DM3
text:
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0219+-0.0014 coming from reactor neutrino experiments, using all solar data and KamLAND data. CPT invariance is assumed.


pdgid: S067DM3
text:
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin**2(theta_{{13}}()) = 0.0219+-0.0014 coming from reactor neutrino experiments, using the Super-Kamiokande-IV data.


pdgid: S067DM3
text:
FORERO 2014 performs a global fit to Deltam(21)**2 using solar, reactor, long-baseline accelerator, and atmospheric neutrino data.


pdgid: S067DM3
text:
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as 7.50+0.19-0.17E-5 eV**2 for normal and 7.50+0.18-0.17E-5 eV**2 for inverted mass ordering.


pdgid: S067DM3
text:
AHARMIM 2013 global solar neutrino data include SNO's all-phases-combined analysis results on the total active B8 neutrino flux and energy-dependent nu_{{e}} survival probability parameters, measurements of Cl (CLEVELAND 1998), Ga (ABDURASHITOV 2009 which contains combined analysis with GNO (ALTMANN 2005 and Ph.D. thesis of F. Kaether)), and Be7 (BELLINI 2011A) rates, and B8 solar-neutrino recoil electron measurements of SK-I (HOSAKA 2006) zenith, SK-II (CRAVENS 2008), and SK-III (ABE 2011) day/night spectra, and Borexino (BELLINI 2010A) spectra.


pdgid: S067DM3
text:
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(31) fixed to 2.45E-3 eV**2, using global solar neutrino data.


pdgid: S067DM3
text:
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(31) fixed to 2.45E-3 eV**2, using global solar neutrino and KamLAND data (GANDO 2011). CPT invariance is assumed.


pdgid: S067DM3
text:
GANDO 2011 obtain this result with three-neutrino fit using the KamLAND data only. Supersedes ABE 2008A.


pdgid: S067DM3
text:
ABE 2008A obtained this result by a rate + shape + time combined geoneutrino and reactor  two-neutrino fit for Deltamass**2(21) and tan**2(theta)(12), using KamLAND data only. Superseded by GANDO 2011.


pdgid: S067DM3
text:
AHARMIM 2008 obtained this result by a two-neutrino oscillation analysis using all solar neutrino data including those of Borexino (ARPESELLA 2008A) and Super-Kamiokande-I (HOSAKA 2006), and KamLAND data (ABE 2008A). CPT invariance is assumed.


pdgid: S067DM3
text:
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (ARAKI 2005). CPT invariance is assumed.


pdgid: S067DM3
text:
HOSAKA 2006 obtained this result from the consistency between the observed and expected day-night flux asymmetry amplitude. The listed 68% CL range is derived from the 1sigma boundary of the amplitude fit to the data. Oscillation parameters are constrained to be in the LMA region. The mixing angle is fixed at tan**2(theta) = 0.44 because the fit depends only very weekly on it.


pdgid: S067DM3
text:
AHARMIM 2005A obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (ARAKI 2005). CPT invariance is assumed. AHARMIM 2005A also quotes Delta(m)**2 = 8.0+0.6-0.4E-5 eV**2 as the error enveloping the 68% CL two-dimensional region.


pdgid: S067DM3
text:
AHARMIM 2005A obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95% CL two-dimensional region shown in figure 35a of AHARMIM 2005A. AHARMIM 2005A also quotes Delta(m)**2 = 6.5+4.4-2.3E-5 eV**2 as the error enveloping the 68% CL two-dimensional region.


pdgid: S067DM3
text:
ARAKI 2005 obtained this result by a two-neutrino oscillation analysis using KamLAND and solar neutrino data. CPT invariance is assumed. The 1sigma error shown here is provided by the KamLAND collaboration. The error quoted in ARAKI 2005, Delta(m)**2 = 7.9+0.6-0.5E-5, envelops the 68% CL two-dimensional region.


pdgid: S067DM3
text:
AHMED 2004A obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (EGUCHI 2003). CPT invariance is assumed. AHMED 2004A also quotes Delta(m)**2 = 7.1+1.2-0.6E-5 eV**2 as the error enveloping the 68% CL two-dimensional region.


pdgid: S067DM3
text:
SMY 2004 obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (IANNI 2003). CPT invariance is assumed.


pdgid: S067P23
text:
ABBASI 2025 uses atmospheric neutrino data measured between 2012 and 2021 with the low-energy subdetector DeepCore of the IceCube neutrino telescope. Supersedes ABBASI 2023.


pdgid: S067P23
text:
ABE 2025B results are based on data collected between 2010 and 2020 in (anti)neutrino mode and include a neutrino beam exposure of 1.97E21 (1.63E21) protons on target. Supersedes ABE 2023F.


pdgid: S067P23
text:
AIELLO 2024 uses atmospheric neutrino data measured between January 2020 and November 2021 with the first six detection units of ORCA, corresponding to 433 kton.yrs.


pdgid: S067P23
text:
WESTER 2024 uses 484.2 kton.years of Super-Kamiokande I-IV atmospheric neutrino data to obtain this result. The fit is performed over the three parameters, Deltam(32)**2, sin**2(theta_{{23}}()), and delta, while the solar parameters and sin**2(theta_{{13}}()) are fixed to Deltam(21)**2 = 7.53+-0.18E-5 eV**2, sin**2(theta_{{12}}()) = 0.307+-0.013, and sin**2(theta_{{13}}()) = 0.0220+-0.0007. Supersedes ABE 2018B.


pdgid: S067P23
text:
ACERO 2022 uses data from Jun 29, 2016 to Feb 26, 2019 (12.5E20 POT) and Feb 6, 2014 to Mar 20, 2020 (13.6E20 POT). Best fit for octant I (lower octant) is 0.46 for both normal and inverted mass orderings. The uncertainties are reported relative to the global minima in normal mass ordering. Supersedes ACERO 2019.


pdgid: S067P23
text:
ADAMSON 2020A uses the complete dataset from MINOS and MINOS+ experiments. The data were collected using a total exposure of 23.76E20 protons on target and 60.75 kton.yr exposure to atmospheric neutrinos. Supersedes ADAMSON 2014.


pdgid: S067P23
text:
ABE 2025 reports the results of a joint analysis of Super-Kamiokande atmospheric neutrino data and T2K beam neutrino data, using 3244.4 days of atmospheric data and a (anti)neutrino beam exposure of 1.97E21 (1.63E21) protons on target.


pdgid: S067P23
text:
ABUBAKAR 2025 results are based on the joint analysis of data sets from NOvA and T2K experiments. The reactor constraint on theta_{{13}} is applied in the fits.


pdgid: S067P23
text:
ACERO 2024 reanalyzed the dataset first examined in ACERO 2022 using an alternative statistical approach based on Bayesian Markov chain Monte Carlo.


pdgid: S067P23
text:
ABBASI 2023 uses atmospheric neutrino data measured between 2011 and 2019 with the low-energy subdetector DeepCore of the IceCube neutrino telescope. Supersedes AARTSEN 2018A.


pdgid: S067P23
text:
ABE 2023D uses the same dataset as ABE 2023F. The measurement of sin**2(theta_{{23}}()) is performed independently for nu_{{mu}} and nubar_{{mu}}.


pdgid: S067P23
text:
ABE 2023F results are based on data collected between 2010 and 2020 in (anti)neutrino mode and include a neutrino beam exposure of 1.97E21 (1.63E21) protons on target. Supersedes ABE 2020F.


pdgid: S067P23
text:
AARTSEN 2020 uses the data taken between May 2012 and April 2014 with the low-energy subdetector DeepCore of the IceCube neutrino telescope. The reconstructed energy range is between 4 (5) and 90 (80) GeV for the main (confirmatory) analysis. Though the observed best-fit is in the lower octant for both mass orderings, a substantial range of sin**2(theta_{{23}}()) > 0.5 is still compatible with the observed data for both mass orderings.


pdgid: S067P23
text:
ABE 2020F results are based on data collected between 2009 and 2018 in (anti)neutrino mode and include a neutrino beam exposure of 1.49E21 (1.64E21) protons on target. Supersedes ABE 2018G.


pdgid: S067P23
text:
AARTSEN 2019C uses three years (April 2012 - May 2015) of neutrino data from full sky with reconstructed energies between 5.6 and 56 GeV, measured with the low-energy subdetector DeepCore of the IceCube neutrino telescope. AARTSEN 2019C adopts looser event selection criteria to prioritize the efficiency of selecting neutrino events, different from tighter event selection criteria which closely follow the criteria used by AARTSEN 2018A to measure the nu_{{mu}} disappearance.


pdgid: S067P23
text:
ACERO 2019 is based on a sample size of 12.33E20 protons on target. The fit combines both antineutrino and neutrino data to extract the oscillation parameters. The results favor the normal mass ordering by 1.9 sigma and theta(23) values in octant II by 1.6 sigma. Supersedes ACERO 2018.


pdgid: S067P23
text:
ALBERT 2019 measured the oscillation parameters of atmospheric neutrinos with the ANTARES deep sea neutrino telescope using the data taken from 2007 to 2016 (2830 days of total live time). Supersedes ADRIAN-MARTINEZ 2012.


pdgid: S067P23
text:
AARTSEN 2018A uses three years (April 2012 - May 2015) of neutrino data from full sky with reconstructed energies between 5.6 and 56 GeV, measured with the low-energy subdetector DeepCore of the IceCube neutrino telescope. AARTSEN 2018A also reports the best fit result for the inverted mass ordering as Deltam(32)**2 = -2.32E-3 eV**2 and sin**2(theta_{{23}}()) = 0.51. Uncertainties for the inverted mass ordering fits were not provided. Supersedes AARTSEN 2015A.


pdgid: S067P23
text:
ABE 2018B uses 328 kton.years of Super-Kamiokande I-IV atmospheric neutrino data to obtain this result. The fit is performed over the four parameters, Deltam(32)**2, sin**2(theta_{{23}}), sin**2(theta_{{13}}), and delta, while the solar parameters are fixed to Deltam(21)**2= 7.53+-0.18E-5 eV**2 and sin**2(theta_{{12}}) = 0.304+-0.014. Superseded by WESTER 2024.


pdgid: S067P23
text:
ABE 2018B uses 328 kton.years of Super-Kamiokande I-IV atmospheric neutrino data to obtain this result. The fit is performed over the three parameters, Deltam(32)**2, sin**2(theta_{{23}}()), and delta, while the solar parameters and sin**2(theta_{{13}}()) are fixed to Deltam(21)**2= 7.53+-0.18E-5 eV**2, sin**2(theta_{{12}}()) = 0.304+-0.014, and sin**2(theta_{{13}}()) = 0.0219+-0.0012. Superseded by WESTER 2024.


pdgid: S067P23
text:
ABE 2018G data prefers normal mass ordering is with a posterior probability of 87%. Supersedes ABE 2017F.


pdgid: S067P23
text:
ACERO 2018 performs a joint fit to the data for nu_{{mu}} disappearance and nu_{{e}} appearance. The overall best fit favors normal mass ordering and theta_{{23}}() in octant II. No 1sigma confidence intervals are presented for the inverted mass ordering scenarios. Superseded by ACERO 2019.


pdgid: S067P23
text:
Errors are from the projections of the 68% contour on 2D plot of Deltam**2 versus sin**2(theta_{{23}}()). ABE 2017F supersedes ABE 2017A. Superseded by ABE 2018G.


pdgid: S067P23
text:
ADAMSON 2016A obtains sin**2(theta_{{23}}()) in the 68% C.L. range [0.38, 0.65] ([0.37, 0.64]), with two statistically degenerate best-fit values of 0.44 and 0.59 (0.44 and 0.59) for normal (inverted) mass ordering. Superseded by ADAMSON 2017A.


pdgid: S067P23
text:
AARTSEN 2015A obtains this result by a three-neutrino oscillation analysis using 10 -- 100 GeV muon neutrino sample from a total of 953 days of measurement with the low-energy subdetector DeepCore of the IceCube neutrino telescope. Superseded by AARTSEN 2018A.


pdgid: S067P23
text:
ABE 2014 results are based on nu_{{mu}} disappearance using three-neutrino oscillation fit. The confidence intervals are derived from one dimensional profiled likelihoods. Superseded by ABE 2017A.


pdgid: S067P23
text:
ADAMSON 2014 uses a complete set of accelerator and atmospheric data. The analysis combines the nu_{{mu}} disappearance and nu_{{e}} appearance data using three-neutrino oscillation fit. The fit results are obtained for normal and inverted mass ordering assumptions. The best fit is for first theta_{{23}}() octant and inverted mass ordering.


pdgid: S067P23
text:
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as 68% CL intervals of 0.433 -- 0.496 or 0.530 -- 0.594 for normal and 0.514 -- 0.612 for inverted mass ordering.


pdgid: S067P23
text:
AARTSEN 2013B obtained this result by a two-neutrino oscillation analysis using 20 -- 100 GeV muon neutrino sample from a total of 318.9 days of live-time measurement with the low-energy subdetector DeepCore of the IceCube neutrino telescope.


pdgid: S067P23
text:
ADAMSON 2013B obtained this result from nu_{{mu}} and nubar_{{mu}} disappearance using nu_{{mu}} (10.71E20 POT) and nubar_{{mu}} (3.36E20 POT) beams, and atmospheric (37.88kton-years) data from MINOS The fit assumed two-flavor neutrino hypothesis and identical nu_{{mu}} and nubar_{{mu}} oscillation parameters. Superseded by ADAMSON 2014.


pdgid: S067P23
text:
ABE 2012A obtained this result by a two-neutrino oscillation analysis. The best-fit point is sin**2(2theta_{{23}}()) = 0.98.


pdgid: S067P23
text:
ADAMSON 2012 is a two-neutrino oscillation analysis using antineutrinos. The best fit value is sin**2(2theta_{{23}}()) = 0.95+0.10-0.11+-0.01.


pdgid: S067P23
text:
ADAMSON 2012B obtained this result by a two-neutrino oscillation analysis of the L/E distribution using 37.9 kton.yr atmospheric neutrino data with the MINOS far detector.


pdgid: S067P23
text:
The best fit point is Deltam**2 = 0.0019 eV**2 and sin**2(2theta) = 0.99. The 90% single-parameter confidence interval at the best fit point is sin**2(2theta) > 0.86.


pdgid: S067P23
text:
The data are separated into pure samples of nu and nubar, and separate oscillation parameters for nu and nubars are fit to the data. The best fit point is (Deltam**2, sin**2(2theta)) = (0.0022 eV**2, 0.99) and (Deltambar**2, sin**2(2thetabar)) = (0.0016 eV**2, 1.00). The quoted result is taken from the 90% C.L. contour in the (Deltam**2, sin**2(2theta)) plane obtained by minimizing the four parameter log-likelihood function with respect to the other oscillation parameters.


pdgid: S067P23
text:
ADRIAN-MARTINEZ 2012 measured the oscillation parameters of atmospheric neutrinos with the ANTARES deep sea neutrino telescope using the data taken from 2007 to 2010 (863 days of total live time). Superseded by ALBERT 2019.


pdgid: S067P23
text:
ABE 2011C obtained this result by a two-neutrino oscillation analysis using the Super-Kamiokande-I+II+III atmospheric neutrino data. ABE 2011C also reported results under a two-neutrino disappearance model with separate mixing parameters between nu and nubar, and obtained sin**2(2theta)> 0.93 for nu and sin**2(2theta)> 0.83 for nubar at 90% C.L.


pdgid: S067P23
text:
ADAMSON 2011B obtained this result by a two-neutrino oscillation analysis of antineutrinos in an antineutrino enhanced beam with 1.71E20 protons on target. This results is consistent with the neutrino measurements of ADAMSON 2011 at 2% C.L.


pdgid: S067P23
text:
WENDELL 2010 obtained this result (sin**2(theta(23)) = 0.407 -- 0.583) by a three-neutrino oscillation analysis using the Super-Kamiokande-I+II+III atmospheric neutrino data, assuming theta(13) = 0 but including the solar oscillation parameters Deltam(21)**2 and sin**2(theta(12)) in the fit.


pdgid: S067P23
text:
WENDELL 2010 obtained this result (sin**2(theta(23)) = 0.43 -- 0.61) by a three-neutrino oscillation analysis with one mass scale dominance (Deltam(21)**2 = 0) using the Super-Kamiokande-I+II+III atmospheric neutrino data, and updates the HOSAKA 2006A result.


pdgid: S067P23
text:
WENDELL 2010 obtained this result (sin**2(theta(23)) = 0.44 -- 0.63) by a three-neutrino oscillation analysis with one mass scale dominance (Deltam(21)**2 = 0) using the Super-Kamiokande-I+II+III atmospheric neutrino data, and updates the HOSAKA 2006A result.


pdgid: S067P23
text:
ADAMSON 2006 obtained this result by a two-neutrino oscillation analysis of the L/E distribution using 4.54 kton yr atmospheric neutrino data with the MINOS far detector.


pdgid: S067P23
text:
ALLISON 2005 result is based upon atmospheric neutrino interactions including upward-stopping muons, with an exposure of 5.9 kton yr. From a two-flavor oscillation analysis the best-fit point is Delta(m**2) = 0.0017 eV**2 and sin**2(2theta) = 0.97.


pdgid: S067P23
text:
ASHIE 2005 obtained this result by a two-neutrino oscillation analysis using 92 kton yr atmospheric neutrino data from the complete Super-Kamiokande I running period.


pdgid: S067P23
text:
AMBROSIO 2004 obtained this result, without using the absolute normalization of the neutrino flux, by combining the angular distribution of upward through-going muon tracks with E_{{mu}} > 1 GeV, N(low) and N(high), and the numbers of InDown + UpStop and InUp events. Here, N(low) and N(high) are the number of events with reconstructed neutrino energies < 30 GeV and > 130 GeV, respectively. InDown and InUp represent events with downward and upward-going tracks starting inside the detector due to neutrino interactions, while UpStop represents entering upward-going tracks which stop in the detector. The best fit is for maximal mixing.


pdgid: S067P23
text:
ASHIE 2004 obtained this result from the L(flight length)/E(estimated neutrino energy) distribution of nu_{{mu}} disappearance probability, using the Super-Kamiokande-I 1489 live-day atmospheric neutrino data.


pdgid: S067P23
text:
There are several islands of allowed region from this K2K analysis, extending to high values of Delta(m**2). We only include the one that overlaps atmospheric neutrino analyses. The best fit is for maximal mixing.


pdgid: S067P23
text:
AMBROSIO 2003 obtained this result on the basis of the ratio R = N(low)/N(high), where N(low) and N(high) are the number of upward through-going muon events with reconstructed neutrino energy < 30 GeV and > 130 GeV, respectively. The data came from the full detector run started in 1994. The method of FELDMAN 1998 is used to obtain the limits.


pdgid: S067P23
text:
AMBROSIO 2003 obtained this result by using the ratio R and the angular distribution of the upward through-going muons. R is given in the previous note and the angular distribution is reported in AMBROSIO 2001. The method of FELDMAN 1998 is used to obtain the limits. The best fit is to maximal mixing.


pdgid: S067P23
text:
SANCHEZ 2003 is based on an exposure of 5.9 kton yr. The result is obtained using a likelihood analysis of the neutrino L/E distribution for a selection mu flavor sample while the e-flavor sample provides flux normalization. The method of FELDMAN 1998 is used to obtain the allowed region. The best fit is sin**2(2theta) = 0.97.


pdgid: S067P23
text:
AMBROSIO 2001 result is based on the angular distribution of upward through-going muon tracks with E_{{mu}} > 1 GeV. The data came from three different detector configurations, but the statistics is largely dominated by the full detector run, from May 1994 to December 2000. The total live time, normalized to the full detector configuration is 6.17 years. The best fit is obtained outside the physical region. The method of FELDMAN 1998 is used to obtain the limits. The best fit is for maximal mixing.


pdgid: S067P23
text:
AMBROSIO 2001 result is based on the angular distribution and normalization of upward through-going muon tracks with E_{{mu}} > 1 GeV. See the previous footnote.


pdgid: S067P23
text:
FUKUDA 1999C obtained this result from a total of 537 live days of upward through-going muon data in Super-Kamiokande between April 1996 to January 1998. With a threshold of E_{{mu}} > 1.6 GeV, the observed flux is 1.74+-0.07+-0.02E-13 cm**-2s**-1sr**-1. The best fit is sin**2(2theta) = 0.95.


pdgid: S067P23
text:
FUKUDA 1999D obtained this result from a simultaneous fitting to zenith angle distributions of upward-stopping and through-going muons. The flux of upward-stopping muons of minimum energy of 1.6 GeV measured between April 1996 and January 1998 is 0.39+-0.04+-0.02E-13 cm**-2s**-1sr**-1. This is compared to the expected flux of (0.73+-0.16 (theoretical error))x10**-13 cm**-2s**-1sr**-1. The best fit is to maximal mixing.


pdgid: S067P23
text:
FUKUDA 1999D obtained this result from the zenith dependence of the upward-stopping/through-going flux ratio. The best fit is to maximal mixing.


pdgid: S067P23
text:
FUKUDA 1998C obtained this result by an analysis of 33.0 kton yr atmospheric neutrino data. The best fit is for maximal mixing.


pdgid: S067P23
text:
HATAKEYAMA 1998 obtained this result from a total of 2456 live days of upward-going muon data in Kamiokande between December 1985 and May 1995. With a threshold of E_{{mu}} > 1.6 GeV, the observed flux of upward through-going muons is 1.94+-0.10+0.07-0.06E-13 cm**-2s**-1sr**-1. This is compared to the expected flux of (2.46+-0.54 (theoretical error))x10**-13 cm**-2s**-1sr**-1. The best fit is for maximal mixing.


pdgid: S067P23
text:
HATAKEYAMA 1998 obtained this result from a combined analysis of Kamiokande contained events (FUKUDA 1994) and upward going muon events. The best fit is sin**2(2theta) = 0.95.


pdgid: S067P23
text:
FUKUDA 1994 obtained the result by a combined analysis of sub- and multi-GeV atmospheric neutrino events in Kamiokande. The best fit is for maximal mixing.


pdgid: S067DM1
text:
JEON 2025 report results derived using the full data set of the RENO reactor anti-neutrino oscillation experiment, conducted at the Hanbit nuclear power plant in Korea. The result summarizes 3800 live days of detector operation. A rate and shape analysis is performed using data collected with near (294 m from reactors) and far detectors (1382 m from reactors). Values of sin**2(theta_{{12}}) and Deltam(21)**2 taken from the 2024 issue of the RPP (PDG 2024) are used to determine these values for both possible mass orderings. This result superseded BAK 2018.


pdgid: S067DM1
text:
AIELLO 2024 reports Deltam(31)**2 = 2.18+0.25-0.35E-3 eV**2 for normal mass ordering. We convert to Deltam(32)**2 using PDG 2024 value of Deltam(21)**2 = 7.53+-0.18E-5 eV**2.


pdgid: S067DM1
text:
AIELLO 2024 reports Deltam(31)**2 = -2.25E-3 to -1.76E-3 eV**2 at 68% CL for inverted mass ordering. We convert to Deltam(32)**2 using PDG 2024 value of Deltam(21)**2 = 7.53+-0.18E-5 eV**2. The inverted mass ordering is disfavored with a p-value of 0.25.


pdgid: S067DM1
text:
AN 2024A report results from 1958 days of data taking with the Daya Bay experiment. This analysis makes use of neutron capture on protons and is independent of previous results in AN 2023, utilizing neutron capture on Gd.


pdgid: S067DM1
text:
AN 2023 reports results derived from the complete data set collected by the Daya-Bay experiment, corresponding to 3158 days of operation, resulting in 5.55E6 nubar_{{e}} candidate events. Solar oscillation parameters are fixed in the analysis to sin**2(theta_{{12}}()) = 0.307+-0.013, Deltam(21)**2 = 7.53+-0.18E-5 eV**2 from PDG 2020. Supersedes ADEY 2018A.


pdgid: S067DM1
text:
ACERO 2022 uses data from Jun 29, 2016 to Feb 26, 2019 (12.5E20 POT) and Feb 6, 2014 to Mar 20, 2020 (13.6E20 POT). For normal mass ordering and theta_{{23}} octant I (lower octant), best fit is 0.00239 eV**2; for inverted mass ordering and octant I, best fit is -0.00244 eV**2. Uncertainties are reported relative to the global minima in normal mass ordering. Supersedes ACERO 2019.


pdgid: S067DM1
text:
ABE 2025 reports |Deltam(13)**2|=2.480+0.052-0.048E-3 eV**2 for inverted mass ordering. We convert to Deltam(32)**2 using PDG 2024 value of Deltam(21)**2 = 7.53+-0.18E-5 eV**2.


pdgid: S067DM1
text:
ABE 2023D uses the same dataset as ABE 2023F. The measurement of Deltam(32)**2 is performed independently for nu_{{mu}} and nubar_{{mu}}.


pdgid: S067DM1
text:
ABE 2023F reports Deltam(13)**2=2.463+0.042-0.056E-3 eV**2 for inverted mass ordering. We convert to Deltam(32)**2 using PDG 2023 value of Deltam(21)**2 = 7.53+-0.18E-5 eV**2.


pdgid: S067DM1
text:
ABE 2020F reports Deltam(13)**2=2.43+-0.07E-3 eV**2 for inverted mass ordering. We convert to Deltam(32)**2 using PDG 2020 value of Deltam(21)**2 = 7.53+-0.18E-5 eV**2.


pdgid: S067DM1
text:
ACERO 2019 is based on a sample size of 12.33E20 protons on target. The fit combines  both antineutrino and neutrino data to extract the oscillation parameters. The results favor the  normal mass ordering by 1.9 sigma and theta(23) values in octant II by 1.6  sigma. Superseded by ACERO 2022.


pdgid: S067DM1
text:
AARTSEN 2018A uses three years (April 2012 - May 2015) of neutrino data from full sky with reconstructed energies between 5.6 and 56 GeV, measured with the low-energy subdetector DeepCore of the IceCube neutrino telescope. AARTSEN 2018A also reports the best fit values for the inverted mass ordering as Deltam(32)**2 = -2.32E-3 eV**2 and sin**2(theta_{{23}}()) = 0.51. Uncertainties for the inverted mass ordering fits were not provided. Supersedes AARTSEN 2015A.


pdgid: S067DM1
text:
ABE 2018B uses 328 kton.years of Super-Kamiokande I-IV atmospheric neutrino data to obtain this result. The fit is performed over the four parameters, Deltam(32)**2, sin**2(theta_{{23}}), sin**2(theta_{{13}}), and delta, while the solar parameters are fixed to Deltam(21)**2= 7.53+-0.18E-5 eV**2 and sin**2(theta_{{12}}) = 0.304+-0.014.


pdgid: S067DM1
text:
ABE 2018G reports Deltam(13)**2=2.432+-0.070E-3 eV**2 for inverted mass ordering. We convert to Deltam(32)**2 using PDG 2018 value of Deltam(21)**2=7.53+-0.18E-5 eV**2.


pdgid: S067DM1
text:
ADEY 2018A reports results from analysis of 1958 days of data taking with the Daya-Bay experiment, with 3.9E6 nubar_{{e}} candidates. The fit to the data gives Deltam(ee)**2 = 2.522+0.068-0.070E-3 eV**2. Solar oscillation parameters are fixed in the analysis using the global averages, sin**2(theta_{{12}}()) = 0.307+0.013-0.012, Deltam(21)**2 = 7.53+-0.18E-5 eV**2, from PDG 2018. Supersedes AN 2017A.


pdgid: S067DM1
text:
BAK 2018 reports results of the RENO experiment using about 2200 live-days of data taken with detectors placed at 410.6 and 1445.7 m from reactors of the Hanbit Nuclear Power Plant. We convert the results to Deltam(32)**2 using the PDG 2018 values of sin**2(theta_{{12}}) = 0.307+0.013-0.012 and Deltam(21)**2 = 7.53+-0.18E-5 eV**2. Supersedes SEO 2018.


pdgid: S067DM1
text:
SEO 2018 reports result of the RENO experiment from a rate and shape analysis of 500 days of data. A simultaneous fit to theta_{{13}} and Deltam(ee)**2 yields Deltam(ee)**2 = 2.62+0.21-0.23+0.12-0.13E-3 eV**2. We convert the results to Deltam(32)**2 using the PDG 2018 values of sin**2(theta_{{12}}) and Deltam(21)**2. SEO 2018 is a detailed description of the results published in CHOI 2016, which it supersedes. Superseded by BAK 2018


pdgid: S067DM1
text:
ABE 2017F confidence intervals are obtained using a frequentist analysis including theta_{{13}} constraint from reactor experiments. Bayesian intervals based on Markov Chain Monte Carlo method are also provided by the authors. Superseded by ABE 2018G.


pdgid: S067DM1
text:
AN 2017A report results from combined rate and spectral shape analysis of 1230 days of data taken with the Daya Bay reactor experiment. The data set contains more than 2.5E6 inverse beta-decay events with neutron capture on Gd. The fit to the data gives Delta(ee)**2=2.50+-0.06+-0.06E-3 eV. Superseded by ADEY 2018A.


pdgid: S067DM1
text:
CHOI 2016 reports result of the RENO experiment from a rate and shape analysis of 500 days of data. A simultaneous fit to theta(13) and Deltam(ee)**2 yields Deltam(ee)**2 = 2.62+0.21-0.23+0.12-0.13E-3 eV. We convert the results to Deltam(32)**2 using PDG 2018 values of sin**2(theta_{{12}}()) and Deltam(21)**2.


pdgid: S067DM1
text:
AARTSEN 2015A obtains this result by a three-neutrino oscillation analysis using 10 -- 100 GeV muon neutrino sample from a total of 953 days of measurements with the low-energy subdetector DeepCore of the IceCube neutrino telescope. Superseded by AARTSEN 2018A.


pdgid: S067DM1
text:
AGAFONOVA 2015A result is based on 5 nu_mu --> nu_tau appearance candidates with an expected background of 0.25+-0.05 events. The best fit is for Deltam(32)**2=3.3E-3 eV**2.


pdgid: S067DM1
text:
AN 2015 uses all eight identical detectors, with four placed near the reactor cores and the remaining four at the far hall to determine prompt energy spectra. The results correspond to the exposure of 6.9E5 GW(th)-ton-days. They derive Deltam(ee)**2 = 2.42+-0.11E-3 eV**2. Assuming the normal (inverted) ordering, the fitted Deltam(32)**2 = 2.37+-0.11E-3 (2.47+-0.11E-3) eV**2. Superseded by AN 2017A.


pdgid: S067DM1
text:
ABE 2014 results are based on nu_{{mu}} disappearance using three-neutrino oscillation fit. The confidence intervals are derived from one dimensional profiled likelihoods. In ABE 2014 the inverted mass ordering result is reported as Deltam(13)**2 = 2.48+-0.10E-3 eV**2 which we converted to Deltam(32)**2 by adding PDG 2014 value of Deltam(21)**2 = 7.53+-0.18E-5 eV**2. Superseded by ABE 2017C.


pdgid: S067DM1
text:
ADAMSON 2014 uses a complete set of accelerator and atmospheric data. The analysis combines The analysis combines the nu_{{mu}} disappearance and nu_{{e}} appearance data using three-neutrino oscillation fit. The fit results are obtained for normal and inverted mass ordering assumptions.


pdgid: S067DM1
text:
AN 2014 uses six identical detectors, with three placed near the reactor cores (flux-weighted baselines of 512 and 561 m) and the remaining three at the far hall (at the flux averaged distance of 1579 m from all six reactor cores) to determine prompt energy spectra and derive  Deltam(ee)**2 = 2.59+0.19-0.20E-3 eV**2. Assuming the normal (inverted)  ordering, the fitted Deltam(32)**2 = 2.54+0.19-0.20E-3 (2.64+0.19-0.20E-3)  eV**2. Superseded by AN 2015.


pdgid: S067DM1
text:
FORERO 2014 performs a global fit to Deltam(31)**2 using solar, reactor, long-baseline accelerator, and atmospheric neutrino data.


pdgid: S067DM1
text:
The value for normal mass ordering is actually a measurement of Deltamass**2(31) which differs from Deltamass**2(32) by a much smaller value of Deltamass**2(12).


pdgid: S067DM1
text:
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as 2.460+-0.046E-3 eV**2 for normal and 2.445+0.047-0.045E-3 eV**2 for inverted mass ordering.


pdgid: S067DM1
text:
Based on the observation of 58 nu_{{mu}} events with 205+-17(syst) expected in the absence of neutrino oscillations. Superseded by ABE 2014.


pdgid: S067DM1
text:
ADAMSON 2013B obtained this result from nu_{{mu}} and nubar_{{mu}} disappearance using nu_{{mu}} (10.71E20 POT) and nubar_{{mu}} (3.36E20 POT) beams, and atmospheric (37.88 kton-years) data from MINOS. The fit assumed two-flavor neutrino hypothesis and identical nu_{{mu}} and nubar_{{mu}} oscillation parameters.


pdgid: S067DM1
text:
ABE 2012A obtained this result by a two-neutrino oscillation analysis. The best-fit point is Deltam(32)**2 = 2.65E-3 eV**2.


pdgid: S067DM1
text:
The 90% single-parameter confidence interval at the best fit point is Deltam**2 = 0.0019+-0.0004 eV**2.


pdgid: S067DM1
text:
ADRIAN-MARTINEZ 2012 measured the oscillation parameters of atmospheric neutrinos with the ANTARES deep sea neutrino telescope using the data taken from 2007 to 2010 (863 days of total live time). Superseded by ALBERT 2019


pdgid: S067DM1
text:
ABE 2011C obtained this result by a two-neutrino oscillation analysis with separate mixing parameters between neutrinos and antineutrinos, using the Super-Kamiokande-I+II+III atmospheric neutrino data. The corresponding 90% CL neutrino oscillation parameter range obtained from this analysis is Deltamass**2() = 1.7 -- 3.0E-3 eV**2.


pdgid: S067DM1
text:
ADAMSON 2011C obtains this result based on a study of antineutrinos in a neutrino beam and assumes maximal mixing in the two-flavor approximation.


pdgid: S067DM1
text:
WENDELL 2010 obtained this result by a three-neutrino oscillation analysis with one mass scale dominance (Deltam(21)**2 = 0) using the Super-Kamiokande-I+II+III atmospheric neutrino data, and updates the HOSAKA 2006A result.


pdgid: S067DM1
text:
ALLISON 2005 result is based on an atmospheric neutrino observation with an exposure of 5.9 kton yr. From a two-flavor oscillation analysis the best-fit point is Delta(m**2) = 0.0017 eV**2 and sin**2(2 theta) = 0.97.


pdgid: S067DM1
text:
ASHIE 2005 obtained this result by a two-neutrino oscillation analysis using 92 kton yr atmospheric neutrino data from the complete Super-Kamiokande I running period. The best fit is for Delta = 2.1E-3 eV**2.


pdgid: S067DM1
text:
AMBROSIO 2004 obtained this result, without using the absolute normalization of the neutrino flux, by combining the angular distribution of upward through-going muon tracks with E_{{mu}} > 1 GeV, N(low) and N(high), and the numbers of InDown + UpStop and InUp events. Here, N(low) and N(high) are the number of events with reconstructed neutrino energies < 30 GeV and > 130 GeV, respectively. InDown and InUp represent events with downward and upward-going tracks starting inside the detector due to neutrino interactions, while UpStop represents entering upward-going tracks which stop in the detector. The best fit is for Delta(m**2) = 2.3E-3 eV**2.


pdgid: S067DM1
text:
ASHIE 2004 obtained this result from the L(flight length)/E(estimated neutrino energy) distribution of nu_{{mu}} disappearance probability, using the Super-Kamiokande-I 1489 live-day atmospheric neutrino data. The best fit is for Delta(m**2) = 2.4E-3 eV**2.


pdgid: S067DM1
text:
There are several islands of allowed region from this K2K analysis, extending to high values of Delta(m**2). We only include the one that overlaps atmospheric neutrino analyses. The best fit is for Delta(m**2) = 2.8E-3 eV**2.


pdgid: S067DM1
text:
AMBROSIO 2003 obtained this result on the basis of the ratio R = N(low)/N(high), where N(low) and N(high) are the number of upward through-going muon events with reconstructed neutrino energy < 30 GeV and > 130 GeV, respectively. The data came from the full detector run started in 1994. The method of FELDMAN 1998 is used to obtain the limits. The best fit is for Delta(m**2) = 2.5E-3 eV**2.


pdgid: S067DM1
text:
AMBROSIO 2003 obtained this result by using the ratio R and the angular distribution of the upward through-going muons. R is given in the previous note and the angular distribution is reported in AMBROSIO 2001. The method of FELDMAN 1998 is used to obtain the limits. The best fit is for Delta(m**2) = 2.5E-3 eV**2.


pdgid: S067DM1
text:
SANCHEZ 2003 is based on an exposure of 5.9 kton yr. The result is obtained using a likelihood analysis of the neutrino L/E distribution for a selection mu flavor sample while the e-flavor sample provides flux normalization. The method of FELDMAN 1998 is used to obtain the allowed region. The best fit is for Delta(m**2) = 5.2E-3 eV**2.


pdgid: S067DM1
text:
AMBROSIO 2001 result is based on the angular distribution of upward through-going muon tracks with E_{{mu}} > 1 GeV. The data came from three different detector configurations, but the statistics is largely dominated by the full detector run, from May 1994 to December 2000. The total live time, normalized to the full detector configuration is 6.17 years. The best fit is obtained outside the physical region. The method of FELDMAN 1998 is used to obtain the limits.


pdgid: S067DM1
text:
FUKUDA 1999C obtained this result from a total of 537 live days of upward through-going muon data in Super-Kamiokande between April 1996 to January 1998. With a threshold of E_{{mu}} > 1.6 GeV, the observed flux is 1.74+-0.07+-0.02E-13 cm**-2s**-1sr**-1. The best fit is for Delta(m**2) = 5.9E-3 eV**2.


pdgid: S067DM1
text:
FUKUDA 1999D obtained this result from a simultaneous fitting to zenith angle distributions of upward-stopping and through-going muons. The flux of upward-stopping muons of minimum energy of 1.6 GeV measured between April 1996 and January 1998 is 0.39+-0.04+-0.02E-13 cm**-2s**-1sr**-1. This is compared to the expected flux of (0.73+-0.16 (theoretical error))x10**-13 cm**-2s**-1sr**-1. The best fit is for Delta(m**2) = 3.9E-3 eV**2.


pdgid: S067DM1
text:
FUKUDA 1999D obtained this result from the zenith dependence of the upward-stopping/through-going flux ratio. The best fit is for Delta(m**2) = 3.1E-3 eV**2.


pdgid: S067DM1
text:
FUKUDA 1998C obtained this result by an analysis of 33.0 kton yr atmospheric neutrino data. The best fit is for Delta(m**2) = 2.2E-3 eV**2.


pdgid: S067DM1
text:
HATAKEYAMA 1998 obtained this result from a total of 2456 live days of upward-going muon data in Kamiokande between December 1985 and May 1995. With a threshold of E_{{mu}} > 1.6 GeV, the observed flux of upward through-going muons is 1.94+-0.10+0.07-0.06E-13 cm**-2s**-1sr**-1. This is compared to the expected flux of (2.46+-0.54 (theoretical error))x10**-13 cm**-2s**-1sr**-1. The best fit is for Delta(m**2) = 2.2E-3 eV**2.


pdgid: S067DM1
text:
HATAKEYAMA 1998 obtained this result from a combined analysis of Kamiokande contained events (FUKUDA 1994) and upward going muon events. The best fit is for Delta(m**2) = 13E-3 eV**2.


pdgid: S067DM1
text:
FUKUDA 1994 obtained the result by a combined analysis of sub- and multi-GeV atmospheric neutrino events in Kamiokande. The best fit is for Delta(m**2) = 16E-3 eV**2.


pdgid: S067P13
text:
JEON 2025 report results derived using the full data set of the RENO reactor anti-neutrino oscillation experiment, conducted at the Hanbit nuclear power plant in Korea. The result summarizes 3800 live days of detector operation. A rate and shape analysis is performed using data collected with near (294 m from reactors) and far detectors (1382 m from reactors). This result superseded BAK 2018 and SHIN 2020.


pdgid: S067P13
text:
ACERO 2024 reanalyzed the NOvA dataset of 13.6E20 POT in neutrino beam node and 12.5E20 POT in antineutrino mode using Bayesian statistical approach. The reported value sin**2(2theta_{{13}})=0.087+0.020-0.016 marginalized over both mass orderings.


pdgid: S067P13
text:
AN 2024A performed a combined analysis of data taken by the Daya Bay experiment. 1958 days use neutron capture on protons, 3158 days neutron capture on Gd, as reported in AN 2023. Combining these data sets results in 8% error reduction compared to AN 2023.


pdgid: S067P13
text:
ABE 2023F results are based on data collected between 2010 and 2020 in (anti)neutrino mode and include a neutrino beam exposure of 1.97E21 (1.63E21) protons on target.


pdgid: S067P13
text:
DE-KERRET 2020 uses 481 days of data from single detector operation and also 384 days of data with both near and far detectors operating. A rate and shape analysis is performed on combined neutron captures on H and Gd. Supersedes ABE 2016B.


pdgid: S067P13
text:
ABUBAKAR 2025 results are based on the joint analysis of data sets from NOvA and T2K experiments. No reactor constraint.


pdgid: S067P13
text:
ABRAHAO 2021 uses 865 days of data collected in both near and far detectors with at least one reactor in operation. The analysis is based on a background model independent approach, so called Reactor Rate Modulation, to determine the mixing angle theta_{{13}}. Adding the background model reduces the uncertainty to 0.0041. Supersedes ABE 2016B.


pdgid: S067P13
text:
SHIN 2020 uses the RENO detector and 1500 live days of data. The near (far) detector observed 567,690 (90,747) nubar_{{e}} candidate events with a delayed neutron capture on hydrogen. The extracted value of sin**2(theta_{{13}}) is consistent with the previous analysis with neutron capture on Gd in BAK 2018.


pdgid: S067P13
text:
AGAFONOVA 2018A reports sin**2(2theta_{{13}}()) < 0.43 at 90% C.L. The result on the sterile neutrino search in the context of 3+1 model is also reported. A 90% C.L. upper limit on sin**2(2thet)(mu e)) = 0.021 for Deltam(41)**2 >= 0.1 eV**2 is set.


pdgid: S067P13
text:
BAK 2018 reports results of the RENO experiment using about 2200 live-days of data taken with detectors placed at 410.6 and 1445.7 m from reactors of the Hanbit Nuclear Power Plant. Supersedes SEO 2018.


pdgid: S067P13
text:
SEO 2018 reports results of the RENO experiment using about 500 days of data, performing a rate and shape analysis. Compared to AHN 2012, a significant reduction of the systematic uncertainties is reported. A 3% excess of events near 5 MeV of the prompt energy is observed. SEO 2018 is a detailed description of the results published in CHOI 2016, which it supersedes. Superseded by BAK 2018.


pdgid: S067P13
text:
Using T2K data only. For inverted mass ordering, all values of theta_{{13}}() are ruled out at 68% CL.


pdgid: S067P13
text:
AN 2017A reports results from combined rate and spectral shape analysis of 1230 days of data taken with the Daya Bay reactor experiment. The data set contains more than 2.5E6 inverse beta-decay events with neutron capture on Gd. A simultaneous fit to theta_{{13}}() and Deltam(ee)**2 is performed. Superseded by ADEY 2018A.


pdgid: S067P13
text:
ABE 2016B uses 455.57 live days of data from a detector 1050 m away from two reactor cores of the Chooz nuclear power station, to determine the mixing parameter sin**2(2theta_{{13}}()). This analysis uses 7.15 reactor-off days for constraining backgrounds. A rate and shape analysis is performed on combined neutron captures on H and Gd. Supersedes ABE 2014H and ABE 2013C.


pdgid: S067P13
text:
AN 2016A uses data from the eight antineutrino detectors (404 days) and six antineutrino detectors (217 days) runs to determine the mixing parameter sin**2(2theta_{{13}}()) using the neutron capture on H only. Supersedes AN 2014B.


pdgid: S067P13
text:
CHOI 2016 reports results of the RENO experiment using about 500 days of data, performing a rate and shape analysis. Compared to AHN 2012, a significant reduction of the systematic uncertainties is reported. A 3% excess of events near 5 MeV of the prompt energy is observed. Supersedes AHN 2012.


pdgid: S067P13
text:
AN 2015 uses all eight identical detectors, with four placed near the reactor cores and the remaining four at the far hall to determine the mixing angle theta(13) using the nubar_{{e}} observed interaction rates with neutron capture on Gd and energy spectra. The result corresponds to the exposure of 6.9E5 GW(th)-ton-days. Superseded by AN 2017A.


pdgid: S067P13
text:
ABE 2014A uses 467.9 live days of one detector, 1050 m away from two reactor cores of the Chooz nuclear power station, to determine the mixing parameter sin**2(2 theta_{{13}}()). The Bugey4 data (DECLAIS 1994) is used to constrain the neutrino flux. The data set includes 7.24 reactor-off days. A "rate-modulation" analysis is performed. Supercedes ABE 2012B.


pdgid: S067P13
text:
ABE 2014C result is for nu_{{e}} appearance and assumes Deltamass**2(32) = 2.4E-3  eV**2, sin**2( theta(23)) = 0.5, and delta = 0.


pdgid: S067P13
text:
ABE 2014H uses 467.9 live days of one detector, 1050 m away from two reactor cores of the Chooz nuclear power station, to determine the mixing parameter sin**2(2 theta_{{13}}()). The Bugey4 data (DECLAIS 1994) is used to constrain the neutrino flux. The data set includes 7.24 reactor-off days. A rate and shape analysis is performed. Superceded by ABE 2016B.


pdgid: S067P13
text:
AN 2014 uses six identical detectors, with three placed near the reactor cores (flux-weighted baselines of 512 and 561 m) and the remaining three at the far hall (at the flux averaged  distance of 1579 m from all six reactor cores) to determine the mixing angle theta(13) using the  nubar_{{e}} observed interaction rates with neutron capture on Gd and energy spectra. Supersedes AN 2013 and superseded by AN 2015.


pdgid: S067P13
text:
AN 2014B uses six identical anti-neutrino detectors with flux-weighted baselines of ~500 m and ~1.6 km to six power reactors. This rate  analysis uses a 217-day data set and neutron capture on protons (not Gd) only. Deltamass**2(31)= 2.32E-3 eV**2 is assumed. Superseded by AN 2016A.


pdgid: S067P13
text:
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as 2.18+0.10-0.11E-2 eV**2 for normal and 2.19+0.12-0.10E-2 eV**2 for inverted mass ordering.


pdgid: S067P13
text:
ABE 2013C uses delayed neutron capture on hydrogen instead of on Gd used previously. The physical volume is thus three times larger. The fit is based on the rate and shape analysis as in ABE 2012B. The Bugey4 data (DECLAIS 1994) is used to constrain the neutrino flux. Superseded by ABE 2016B.


pdgid: S067P13
text:
ADAMSON 2013A results obtained from nu_{{e}} appearance, assuming delta = 0, and sin**2(2 theta(23)) = 0.957.


pdgid: S067P13
text:
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(32) fixed to 2.45E-3 eV**2, using global solar neutrino data. AHARMIM 2013 global solar neutrino data include SNO's all-phases-combined analysis results on the total active B8 neutrino flux and energy-dependent nu_{{e}} survival probability parameters, measurements of Cl (CLEVELAND 1998), Ga (ABDURASHITOV 2009 which contains combined analysis with GNO (ALTMANN 2005 and Ph.D. thesis of F. Kaether)), and Be7 (BELLINI 2011A) rates, and B8 solar-neutrino recoil electron measurements of SK-I (HOSAKA 2006) zenith, SK-II (CRAVENS 2008) and SK-III (ABE 2011) day/night spectra, and Borexino (BELLINI 2010A) spectra. AHARMIM 2013 also reported a result combining global solar and KamLAND data, which is sin**2(2 theta_{{13}}()) = 9.1+2.9-3.1E-2.


pdgid: S067P13
text:
AN 2013 uses six identical detectors, with three placed near the reactor cores (flux-weighted baselines of 498 and 555 m) and the remaining three at the far hall (at the flux averaged distance of 1628 m from all six reactor cores) to determine the nubar_{{e}} interaction rate ratios. Superseded by AN 2014.


pdgid: S067P13
text:
ABE 2012 determines the nubar_{{e}} interaction rate in a single detector, located 1050 m from the cores of two reactors. A rate and shape analysis is performed. The rate normalization is fixed by the results of the Bugey4 reactor experiment, thus avoiding any dependence on possible very short baseline oscillations. The value of Deltamass**2(31) = 2.4E-3 eV**2 is used in the analysis. Superseded by ABE 2012B.


pdgid: S067P13
text:
ABE 2012B determines the neutrino mixing angle theta_{{13}}() using a single detector, located 1050 m from the cores of two reactors. This result is based on a spectral shape and rate analysis. The Bugey4 data (DECLAIS 1994) is used to constrain the neutrino flux. Superseded by ABE 2014A.


pdgid: S067P13
text:
AHN 2012 uses two identical detectors, placed at flux weighted distances of 408.56 m and 1433.99 m from six reactor cores, to determine the mixing angle theta_{{13}}. This rate-only analysis excludes the no-oscillation hypothesis at 4.9 standard deviations. The value of Deltamass**2(31) = 2.32+0.12-0.08E-3 eV**2 was assumed in the analysis. Superseded by CHOI 2016.


pdgid: S067P13
text:
AN 2012 uses six identical detectors with three placed near the reactor cores (flux-weighted baselines of 470 m and 576 m) and the remaining three at the far hall (at the flux averaged distance of 1648 m from all six reactor cores) to determine the mixing angle theta_{{13}} using the nubar_{{e}} observed interaction rate ratios. This rate-only analysis excludes the no-oscillation hypothesis at 5.2 standard deviations. The value of Deltamass**2(31)  = 2.32+0.12-0.08E-3 eV**2 was assumed in the analysis. Superseded by AN 2013.


pdgid: S067P13
text:
ABE 2011 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(32) fixed to 2.4E-3 eV**2, using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, SAGE, and KamLAND data. This result implies an upper bound of sin**2(theta_{{13}})< 0.059 (95% CL) or sin**2(2theta_{{13}})< 0.22 (95% CL). The normal neutrino mass ordering and CPT invariance are assumed.


pdgid: S067P13
text:
The quoted limit is for Deltamass**2(32) = 2.4E-3 eV**2, theta(23) = pi/2, delta = 0, and the normal mass ordering. For other values of delta, the 68% region spans from 0.03 to 0.25, and the 90% region from 0.02 to 0.32.


pdgid: S067P13
text:
The quoted limit is for Deltamass**2(32) = 2.4E-3 eV**2, theta(23) = pi/2, delta = 0, and the inverted mass ordering. For other values of delta, the 68% region spans from 0.04 to 0.30, and the 90% region from 0.02 to 0.39.


pdgid: S067P13
text:
The quoted limit is for Deltamass**2(32) = 2.32E-3 eV**2, theta(23) = pi/2, delta = 0, and the normal mass ordering. For other values of delta, the 68% region spans from 0.02 to 0.12, and the 90% region from 0 to 0.16.


pdgid: S067P13
text:
The quoted limit is for Deltamass**2(32) = 2.32E-3 eV**2, theta(23) = pi/2, delta = 0, and the inverted mass ordering. For other values of delta, the 68% region spans from 0.02 to 0.16, and the 90% region from 0 to 0.21.


pdgid: S067P13
text:
FOGLI 2011 obtained this result from an analysis using the atmospheric, accelerator long baseline, CHOOZ, solar, and KamLAND data. Recently, MUELLER 2011 suggested an average increase of about 3.5% in normalization of the reactor nubar_{{e}} fluxess, and using these fluxes, the fitted result becomes 0.10+-0.03.


pdgid: S067P13
text:
GANDO 2011 report sin**2(theta_{{13}}()) = 0.020+-0.016. This result was obtained with three-neutrino fit using the KamLAND + solar data.


pdgid: S067P13
text:
GANDO 2011 report sin**2(theta_{{13}}()) = 0.032+-0.037. This result was obtained with three-neutrino fit using the KamLAND data only.


pdgid: S067P13
text:
This result corresponds to the limit of <0.12 at 90% CL for Deltam(32)**2 = 2.43E-3 eV**2, theta(23) = pi/2, and delta = 0. For other values of delta, the 90% CL region spans from 0 to 0.16.


pdgid: S067P13
text:
This result corresponds to the limit of <0.20 at 90% CL for Deltam(32)**2 = 2.43E-3 eV**2, theta(23) = pi/2, and delta = 0. For other values of delta, the 90% CL region spans from 0 to 0.21.


pdgid: S067P13
text:
AHARMIM 2010 obtained this result by a three-neutrino oscillation analysis with the value of Deltamass**2(31) fixed to 2.3E-3 eV**2, using global solar neutrino data and KamLAND data (ABE 2008A). CPT invariance is assumed. This result implies an upper bound of sin**2(theta_{{13}}())< 0.057 (95% CL) or sin**2(2theta_{{13}}())< 0.22 (95% CL).


pdgid: S067P13
text:
The quoted limit is for Deltam(32)**2 = 2.43E-3 eV**2, theta(23) = pi/2, and delta = 0. For other values of delta, the 68% CL region spans from 0.02 to 0.26.


pdgid: S067P13
text:
The quoted limit is for Deltam(32)**2 = 2.43E-3 eV**2, theta(23) = pi/2, and delta = 0. For other values of delta, the 68% CL region spans from 0.04 to 0.34.


pdgid: S067P13
text:
FOGLI 2008 obtained this result from a global analysis of all neutrino oscillation data, that is, solar + KamLAND + atmospheric + accelerator long baseline + CHOOZ.


pdgid: S067P13
text:
FOGLI 2008 obtained this result from an analysis using the solar and KamLAND neutrino oscillation data.


pdgid: S067P13
text:
FOGLI 2008 obtained this result from an analysis using the atmospheric, accelerator long baseline, and CHOOZ neutrino oscillation data.


pdgid: S067P13
text:
YAMAMOTO 2006 searched for nu_mu --> nu_e appearance. Assumes 2 sin**2(2theta(mu e)) = sin**2(2theta(13)). The quoted limit is for Deltam(32)**2 = 1.9E-3 eV**2. That value of Deltam(32)**2 is the one-sigma low value for AHN 2006A. For the AHN 2006A best fit value of 2.8E-3 eV**2, the sin**2(2theta(13)) limit is < 0.26. Supersedes AHN 2004.


pdgid: S067P13
text:
AHN 2004 searched for nu_mu --> nu_e appearance. Assuming 2 sin**2(2 theta(mu_{{e}})) = sin**2(2 theta(13)), a limit on sin**2(2 theta(mu_{{e}})) is converted to a limit on sin**2(2 theta(13)).The quoted limit is for Deltam(32)**2 = 1.9E-3 eV**2. That value of Deltam(32)**2 is the one-sigma low value for ALIU 2005. For the ALIU 2005 best fit value of 2.8E-3 eV**2, the sin**2(2 theta(13)) limit is < 0.30.


pdgid: S067P13
text:
The quoted limit is for Delta(m)(32)**2 = 1.9E-3 eV**2. That value of Delta(m)(32)**2 is the 1-sigma low value for ALIU 2005. For the ALIU 2005 best fit value of 2.8E-3 eV**2, the sin**2(2 theta)(13) limit is < 0.19. In this range, the theta(13) limit is larger for lower values of Delta(m)(32)**2, and smaller for higher values of Delta(m)(32)**2.


pdgid: S067P13
text:
The quoted limit is for Delta(m)(32)**2 = 1.9E-3 eV**2. That value of Delta(m)(32)**2 is the 1-sigma low value for ALIU 2005. For the ALIU 2005 best fit value of 2.8E-3 eV**2, the sin**2(2 theta)(13) limit is < 0.23.


pdgid: S067P13
text:
The quoted limit is for Delta(m)(32)**2 = 2.43E-3 eV**2. That value of Delta(m)(32)**2 is the central value for ADAMSON 2008. For the ADAMSON 2008 1-sigma low value of 2.30E-3 eV**2, the sin**2(2 theta)(13) limit is < 0.16. See also APOLLONIO 2003 for a detailed description of the experiment.


pdgid: S067DEL
text:
ABE 2025B results are based on data collected between 2010 and 2020 in (anti)neutrino mode and include a neutrino beam exposure of 1.97E21 (1.63E21) protons on target. For inverted mass ordering, the quoted result is 1.54+0.18-0.19 pi rad. Supersedes ABE 2023F.


pdgid: S067DEL
text:
For the octant I (lower octant), the 68% CL allowed region is discontinuous, and all delta values are allowed at 90% CL.


pdgid: S067DEL
text:
ACERO 2022 uses data from Jun 29, 2016 to Feb 26, 2019 (12.5E20 POT) and Feb 6, 2014 to Mar 20, 2020 (13.6E20 POT). Results for normal and inverted mass ordering, and  theta_{{23}}()  octant I and II are presented. Supersedes ACERO 2019.


pdgid: S067DEL
text:
ABE 2023F results are based on data collected between 2010 and 2020 in (anti)neutrino mode and include a neutrino beam exposure of 1.97E21 (1.63E21) protons on target. For inverted mass ordering, the quoted result is 1.54+0.18-0.19 pi rad. Supersedes ABE 2020F.


pdgid: S067DEL
text:
The inverted mass ordering is rejected at 1.0 sigma. The error bars are reported relative to the global minima in normal mass ordering.


pdgid: S067DEL
text:
SALAS 2021 reports results of a global fit to neutrino oscillation data available at the  time of the Neutrino 2020 conference.


pdgid: S067DEL
text:
ABE 2020F results are based on data collected between 2009 and 2018 in (anti)neutrino mode and include a neutrino beam exposure of 1.49E21 (1.64E21) protons on target. For inverted mass ordering, the quoted result is 1.56+0.15-0.17 pi rad. Supersedes ABE 2018G.


pdgid: S067DEL
text:
ESTEBAN 2020A reports results of a global fit to neutrino oscillation data available at the  time of the Neutrino 2020 conference.


pdgid: S067DEL
text:
ACERO 2019 is based on a sample size of 1.33E20 protons on target with combined  antineutrino and neutrino data. Superseded by ACERO 2022.


pdgid: S067DEL
text:
ABE 2018B uses 328 kton.years of Super-Kamiokande I-IV atmospheric neutrino data to obtain this result. The fit is performed over the three parameters, Deltam(32)**2, sin**2(theta_{{23}}), and delta, while the solar parameters and sin**2(theta_{{23}}) are fixed to Deltam(21)**2= 7.53+-0.18E-5 eV**2, sin**2(theta_{{12}}) = 0.304+-0.014, and sin**2(theta_{{13}}) = 0.0219+-0.0012.  Superseded by WESTER 2024.


pdgid: S067DEL
text:
ABE 2018G confidence intervals are marginalized over both mass orderings. Normal order preferred with a posterior probability of 87%. The 1-sigma result for normal mass ordering used in the average was provided by the experiment via private communications. Supersedes ABE 2017F.


pdgid: S067DEL
text:
ADAMSON 2016 result is based on a data sample with 2.74E20 protons on target. The likelihood-based analysis observed 6 nu_{{e}} events with an expected background of 0.99+-0.11 events.


pdgid: S067DEL
text:
ADAMSON 2014 result is based on three-flavor formalism and theta_{{23}}()>pi/4. Likelihood as a function of delta is also shown for the other three combinations of hierarchy and theta_{{23}}() octants; all values of delta are allowed at 90% C.L.


pdgid: S067DEL
text:
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as 68% CL intervals of 1.24 -- 1.94 for normal and 1.15 -- 1.77 for inverted mass ordering.


pdgid: S067DEL
text:
ADAMSON 2013A result is based on nu_{{e}} appearance in MINOS and the calculated sin**2(2theta_{{23}}()) = 0.957,theta_{{23}}()>pi/4, and normal mass hierarchy. Likelihood as a function ofdelta is also shown for the other three combinations of hierarchy and theta_{{23}}() octants; all values of delta are allowed at 90% C.L.


pdgid: S067D1
text:
AGUILAR-AREVALO 2021 result is based on a total of 18.75E20 POT in neutrino mode, and 11.27E20 POT in anti-neutrino mode. Best fit at 0.043 eV**2. The allowed region does not extend to large Deltam**2. The quoted value is the entire allowed region of Deltam**2 at 90% C.L. for all values of sin**2(2theta). Supersedes AGUILAR-AREVALO 2018C.


pdgid: S067D1
text:
AGUILAR-AREVALO 2018C result is based on nu_mu --> nu_e appearance of 460.5+-99.0  events; The best fit value is Deltam**2 = 0.041 eV**2. Superseded by AGUILAR-AREVALO 2021.


pdgid: S067D1
text:
AGUILAR-AREVALO 2013A result is based on nu_mu --> nu_e appearance of 162.0+-47.8 events; marginally compatible with twoneutrino oscillations. The best fit value is Deltam**2 = 3.14 eV**2.


pdgid: S067D1
text:
MAHN 2012 is a combined spectral fit of MiniBooNE and SciBooNE neutrino data with the range of Deltam**2 up to 25 eV**2. The best limit is 0.04 at 7 eV**2.


pdgid: S067D1
text:
AGUILAR 2001 is the final analysis of the LSND full data set. Search is made for the nu_mu --> nu_e oscillations using nu_{{mu}} from pi+ decay in flight by observing beam-on electron events from nu_e ^C --> e- X. Present analysis results in 8.1+-12.2+-1.7 excess events in the 60<E(e)<200 MeV energy range, corresponding to oscillation probability of 0.10+-0.16+-0.04%. This is consistent, though less significant, with the previous result of ATHANASSOPOULOS 1998, which it supersedes. The present analysis uses selection criteria developed for the decay at rest region, and is less effective in removing the background above 60 MeV than ATHANASSOPOULOS 1998.


pdgid: S067D1
text:
ATHANASSOPOULOS 1998 is a search for the nu_mu --> nu_e oscillations using nu_{{mu}} from pi+ decay in flight. The 40 observed beam-on electron events are consistent with nu_e ^C --> e- X; the expected background is 21.9+-2.1. Authors interpret this excess as evidence for an oscillation signal corresponding to oscillations with probability (0.26+-0.10+-0.05)%. Although the significance is only 2.3 sigma, this measurement is an important and consistent cross check of ATHANASSOPOULOS 1996 who reported evidence for nubar_mu --> nubar_e oscillations from mu+ decay at rest. See also ATHANASSOPOULOS 1998B.


pdgid: S067D1
text:
LOVERRE 1996 uses the charged-current to neutral-current ratio from the combined CHARM (ALLABY 1986) and CDHS (ABRAMOWICZ 1986) data from 1986.


pdgid: S067S1
text:
AGUILAR-AREVALO 2021 result is based on a total of 18.75E20 POT in neutrino mode, and 11.27E20 POT in anti-neutrino mode. The best fit value is sin**2(2theta)=0.807. The allowed region does not extend to large Delta. The quoted value is the entire allowed region of sin**2(2theta) at 90% C.L. for all values of Delta. Supersedes AGUILAR-AREVALO 2018C.


pdgid: S067S1
text:
AGUILAR-AREVALO 2018C result is based on nu_mu --> nu_e appearance of 460.5+-99.0  events; The best fit value is sin**2(2theta) = 0.92. The quoted limit for the two-neutrino mixing angle theta is valid above Deltam**2 = 0.59 eV**2. Superseded by AGUILAR-AREVALO 2021.


pdgid: S067S1
text:
AGUILAR-AREVALO 2013A result is based on nu_mu --> nu_e appearance of 162.0+-47.8 events; marginally compatible with two neutrino oscillations. The best fit value is sin**2(2theta) = 0.002.


pdgid: S067S1
text:
ANTONELLO 2013 use the ICARUS T600 detector at LNGS and ~20 GeV beam of nu_{{mu}} from CERN 730 km away to search for an excess of nu_{{e}} events. Two events are found with 3.7+-0.6 expected from conventional sources. This result excludes some parts of the parameter space expected by LSND. Superseded by ANTONELLO 2013A.


pdgid: S067S1
text:
Based on four events with a background of 6.4+-0.9 from conventional sources with an average energy of 20 GeV and 730 km from the source of nu_{{mu}}.


pdgid: S067S1
text:
The limit is sin**2(2theta) < 0.9E-3 at Delta = 2 eV**2. That value of Delta corresponds to the smallest mixing angle consistent with the reported signal from LSND in AGUILAR 2001.


pdgid: S067S1
text:
The limit becomes sin**2(2theta) < 0.15 at Delta = 2.8E-3 eV**2, the bets-fit value of the nu_{{mu}} disappearance analysis in K2K.


pdgid: S067S1
text:
AGUILAR 2001 is the final analysis of the LSND full data set of the search for the nu_mu --> nu_e oscillations. See footnote in preceding table for further details.


pdgid: S067S1
text:
ATHANASSOPOULOS 1998 report (0.26+-0.10+-0.05)% for the oscillation probability; the value of sin**2(2theta) for large Deltam**2 is deduced from this probability. See footnote in preceding table for further details, and see the paper for a plot showing allowed regions. If effect is due to oscillation, it is most likely to be intermediate sin**2(2theta) and Deltam**2. See also ATHANASSOPOULOS 1998B.


pdgid: S067S1
text:
VILAIN 1994C limit derived by combining the nu_{{mu}} and nubar_{{mu}} data assuming CP conservation.


pdgid: S067D2
text:
Based on nubar_mu --> nubar_e appearance of 78.4+-28.5 events. The best fit values are Deltam**2 = 0.043 eV**2 and sin**2(2theta) = 0.88.


pdgid: S067D2
text:
This value is for a two neutrino oscillation analysis for excess antineutrino events with E(nu)> 475 MeV. The best fit is at 0.07. The allowed region is consistent with LSND reported by AGUILAR 2001. Supercedes AGUILAR-AREVALO 2009B.


pdgid: S067D2
text:
This value is for a two neutrino oscillation analysis for excess antineutrino events with E(nu)> 200 MeV with subtraction of the expected 12 events low energy excess seen in the neutrino component of the beam. The best fit value is 0.007 for Delta(m)**2 = 4.4 eV**2.


pdgid: S067D2
text:
ARMBRUSTER 2002 is the final analysis of the KARMEN 2 data for 17.7 m distance from the ISIS stopped pion and muon neutrino source. It is a search for nubar_{{e}}, detected by the inverse beta-decay reaction on protons and C12. 15 candidate events are observed, and 15.8+-0.5 background events are expected, hence no oscillation signal is detected. The results exclude large regions of the parameter area favored by the LSND experiment.


pdgid: S067D2
text:
AGUILAR 2001 is the final analysis of the LSND full data set. It is a search for nubar_{{e}} 30 m from LAMPF beam stop. Neutrinos originate mainly for pi+ decay at rest. nubar_{{e}} are detected through nubar_e p --> e+ n (20<E(e+)<60 MeV) in delayed coincidence with n p --> d gamma. Authors observe 87.9+-22.4+-6.0 total excess events. The observation is attributed to nubar_mu --> nubar_e oscillations with the oscillation probability of 0.264+-0.067+-0.045%, consistent with the previously published result. Taking into account all constraints, the most favored allowed region of oscillation parameters is a band of Delta(m)**2 from 0.2 -- 2.0 eV**2. Supersedes ATHANASSOPOULOS 1995, ATHANASSOPOULOS 1996, and ATHANASSOPOULOS 1998.


pdgid: S067D2
text:
ATHANASSOPOULOS 1996 is a search for nubar_{{e}} 30 m from LAMPF beam stop. Neutrinos originate mainly from pi+ decay at rest. nubar_{{e}} could come from either nubar_mu --> nubar_e or nu_e --> nubar_e; our entry assumes the first interpretation. They are detected through nubar_e p --> e+ n (20 MeV <E(e+)<60 MeV) in delayed coincidence with n p --> d gamma. Authors observe 51+-20+-8 total excess events over an estimated background 12.5+-2.9. ATHANASSOPOULOS 1996B is a shorter version of this paper.


pdgid: S067D2
text:
ATHANASSOPOULOS 1995 error corresponds to the 1.6sigma band in the plot. The expected background is 2.7+-0.4 events. Corresponds to an oscillation probability of (0.34+0.20-0.18+-0.07)%. For a different interpretation, see HILL 1995. Replaced by ATHANASSOPOULOS 1996.


pdgid: S067D2
text:
HILL 1995 is a report by one member of the LSND Collaboration, reporting a different conclusion from the analysis of the data of this experiment (see ATHANASSOPOULOS 1995). Contrary to the rest of the LSND Collaboration, Hill finds no evidence for the neutrino oscillation nubar_mu --> nubar_e and obtains only upper limits.


pdgid: S067D2
text:
FREEDMAN 1993 is a search at LAMPF for nubar_{{e}} generated from any of the three neutrino types nu_{{mu}}, nubar_{{mu}}, and nu_{{e}} which come from the beam stop. The nubar_{{e}}'s would be detected by the reaction nubar_e p --> e+ n. FREEDMAN 1993 replaces DURKIN 1988.


pdgid: S067S2
text:
ANTONELLO 2013A obtained the limit by assuming nubar_mu --> nubar_e oscillation from the ~2% of nubar_{{mu}} evnets contamination in the CNGS beam.


pdgid: S067S2
text:
This value is for a two neutrino oscillation analysis for excess antineutrino events with E(nu)> 475 MeV. At 90% CL there is no solution at high Delta(m)**2. The best fit is at maximal mixing. The allowed region is consistent with LSND reported by AGUILAR 2001. Supercedes AGUILAR-AREVALO 2009B.


pdgid: S067S2
text:
This value is for a two neutrino oscillation analysis for excess antineutrino events with E(nu)> 200 MeV with subtraction of the expected 12 events low energy excess seen in the neutrino component of the beam. At 90% CL there is no solution at high Delta(m)**2. The best fit value is 0.007 for Delta(m)**2 = 4.4 eV**2.


pdgid: S067S2
text:
ARMBRUSTER 2002 is the final analysis of the KARMEN 2 data. See footnote in the preceding table for further details, and the paper for the exclusion plot.


pdgid: S067S2
text:
AGUILAR 2001 is the final analysis of the LSND full data set. The deduced oscillation probability is 0.264+-0.067+-0.045%; the value of sin**2(2theta) for large Delta(m)**2 is twice this probability (although these values are excluded by other constraints). See footnote in preceding table for further details, and the paper for a plot showing allowed regions. Supersedes ATHANASSOPOULOS 1995, ATHANASSOPOULOS 1996, and ATHANASSOPOULOS 1998.


pdgid: S067S2
text:
ATHANASSOPOULOS 1996 reports (0.31+-0.12+-0.05)% for the oscillation probability; the value of sin**2(2theta) for large Delta(m)**2 should be twice this probability. See footnote in preceding table for further details, and see the paper for a plot showing allowed regions.


pdgid: S067DU4
text:
OYAMA 1989 gives a range of limits, depending on assumptions in their analysis. They argue that the region Delta(m)**2 = (100-1000)*10**-5 eV**2 is not ruled out by any data for large mixing.


pdgid: S067NUS
text:
ACHARYA 2025D analyze 3.6E7 tritium beta decay events, collected by the KATRIN experiment, to place a limit on the admixture of sterile neutrinos. A 3+1 neutrino mixing model is assumed. The value reported here corresponds to approximately Deltam(41)**2 ~ 300 eV**2, where their sensitivity is maximal in a two-dimensional Deltam(41)**2 versus sin**2(2theta(ee)) plot. We convert the limit to sin**2(theta(ee)).


pdgid: S067NUS
text:
ANDRIAMIRADO 2025 report results derived from the complete dataset collected by the PROSPECT-I detector in 2018. Their disappearance search for nubar_e --> nubar_s oscillations at 7 -- 9 m distance to the HFIR reactor at ORNL shows no evidence for oscillations. The data is interpreted in a 3+1 mixing model and results are reported in a Deltam(41)**2 versus sin**2(2theta(14)) exclusion plot. The most sensitive sin**2(2theta(14)) exclusion is reported here. It is taken from figure 4 and corresponds to Deltam(41)**2 at ~ 3 eV**2.


pdgid: S067NUS
text:
AN 2024 use the full data set of the Daya Bay reactor experiment, corresponding to 3158 days of detector operation, to place a limit on nubar_e --> nubar_s oscillations. The result is in terms of sin**2(2theta(14)) for 0.01 eV**2 < Deltam(41)**2 < 0.1 eV**2. A 3+1 mixing model is assumed.


pdgid: S067NUS
text:
AUGIER 2024 use of 1.47 kg.yr of Mo100 exposure of the CUPID-Mo scintillating cryogenic calorimeter, operated at the Laboratoire Souterrain de Modane, to place a range of limits on the admixture of sterile neutrinos. Two different 2nubeta beta spectral analysis approaches are used. sin**2(theta(14)) is given for sterile neutrino masses ranging from 0.5 to 1.5 MeV. The limit above is for 0.5 MeV mass.


pdgid: S067NUS
text:
AKER 2023 assume a 3+1 neutrino mixing model, use low-rate commissioning data of the KATRIN tritium beta decay experiment to place a limit on sin**2(theta(14)) for a admixture sterile neutrino mass m(4) of ~ 300 eV.


pdgid: S067NUS
text:
ALMAZAN 2023 use inverse beta decay data collected by the STEREO experiment, placed 9 to 11 m  from the ILL research reactor, to search for nubar_e --> nubar_s oscillations. The ILL research reactor uses highly enriched U235 fuel. No indication of the oscillation to sterile neutrinos is found, the stated limit on sin**2(2theta(14)) correspond to  Deltam(41)**2 ~ 1 eV**2 where the exclusion is maximal. Supersedes  ALMAZAN 2018.


pdgid: S067NUS
text:
AKER 2022A uses the first two science runs of the KATRIN tritium beta decay neutrino mass experiment to search for an admixture of sterile neutrinos. No evidence is found for a spectral anomaly, indicating such admixture. The resulting limit is on sin**2(2theta(14)) for sterile neutrino masses m(4) < 40 eV. It is most restrictive at Deltam(41)**2 ~ 400 eV**2. A 3+1 model is assumed.


pdgid: S067NUS
text:
ATIF 2022 report results from the combined analysis of the RENO (419 m) and NEOS (24 m) experiments data, collected at the Hanbit Nuclear Power Plant. Results, in terms of sin**2(2theta(14)), constrain for nubar_e --> nubar_s oscillations. The authors report both excluded and allowed parameter combinations. The exclusion result reported here is based on the Feldman-Cousins method and for Deltam(41)**2 ~ 0.55 eV**2. Part of the allowed area is excluded by the STEREO and PROSPECT experiments.


pdgid: S067NUS
text:
BARINOV 2022A report an event deficit observed using the segmented Baksan Ga neutrino  detector, exposed to a 3.4 MCi Cr51 source. Equal suppression factors are observed for  the inner and outer segments. The deficit is interpreted as evidence for oscillations to sterile  neutrinos. The result is in terms of sin**2(2theta(14)), for a best fit of  Deltam(41)**2 =3.3 (-2.3)**+inf eV**2. Some, but not all, of the allowed neutrino parameter space conflicts with other experiments.


pdgid: S067NUS
text:
ANDRIAMIRADO 2021 reports a search for nubar_e --> nubar_s oscillations at the HFIR research reactor, at baselines from 6.7 to 9.2 m. The reactor has a U235 core. 4 tons of Li6-doped liquid scintillator are used in a segmented detector. Oscillations into sterile neutrinos are disfavored. The stated limit for sin**2(2theta(14)) is for Deltam(41)**2 ~ 2 eV**2 where the sensitivity is maximal.


pdgid: S067NUS
text:
SEREBROV 2021 searches for nubar_e --> nubar_s oscillations with a moveable detector with baseline 6 -- 12 m from the SM-3 research reactor with highly enriched U235 fuel.  Analyzing the L/E dependence a chi^2 minimum is found at Deltam(41)**2 = 7.3+-0.13+-1.16 eV**2 and sin**2(2theta(14)) = 0.36+-0.12. The quoted limit of 0.005 for sin**2(2theta(14)) corresponds to Deltam(41)**2 ~ 2 eV**2. This is the result from 720 days of reactor ON and 860 days of reactor OFF measurements. The significance of the chi^2 minimum is 2.9 sigma. Supersedes SEREBROV 2020, SEREBROV 2019 and SEREBROV 2018A.


pdgid: S067NUS
text:
SKROBOVA 2020 searches for nubar_{{e}}-nubar_{{s}} oscillations using the DANSS detector at 10.7, 11.2, and 12.7 m from the 3.1 GW(th) power reactor. The DANSS detector is highly segmented and moveable; the positions are changed usually 3 times a week. The analysis is based on the ratio of the events at top and bottom position; the middle position is used for checks of consistency. No evidence for sterile neutrinos is found. The quoted limit 0.008, the smallest excluded sin**2(2theta(14)), corresponds to Deltam(41)**2 ~ 1.0 eV**2. Supersedes ALEKSEEV 2018.


pdgid: S067NUS
text:
ALEKSEEV 2018 searches for nubar_e --> nubar_s oscillations using the DANSS detector at   10.7, 11.2, and 12.7 m from the 3.1 GW(th) power reactor. The DANSS detector is highly   segmented and moveable; the positions are changed usually 3 times a week. The analysis is based on   the ratio of the events at top and bottom position; the middle position is used for checks of   consistency. The best fit point is at Deltam(41)**2 = 1.4 eV**2 and   sin**2(2theta(14)) = 0.05 with Deltachi**2 = 13.1 (statistical   errors only) compared to the fit with 3 active neutrinos only. The quoted limit of 0.01 for   sin**2(2theta(14)) corresponds to Deltam(41)**2 ~ 1.0 eV**2.  Superseded by SKROBOVA 2020.


pdgid: S067NUS
text:
ALMAZAN 2018 searches for the nubar_e --> nubar_s oscillations with baseline from 9.4 to  11.1 m from the ILL research reactor with highly enriched U235 fuel. The STEREO detector consists of six separated cells with Gd loaded scintillator, with 15 m water equivalent overburden. The detected rate is 396.3+-4.7 nubar_{{e}}/day with signal to background ratio of about 0.9. The reported results corresponds to 66 days of reactor-on. The analysis uses the relative rates normalized to the cell number 1. No indication of the oscillation to the sterile neutrinos is found, the stated limit on sin**2(2theta(14)) correspond to Deltam**2(41) ~ 3.5 eV**2 where the exclusion is maximal. Superseded by ALMAZAN 2023.


pdgid: S067NUS
text:
ASHENFELTER 2018 searches for the nubar_e --> nubar_s oscillations at baseline from 6.7 to 9.2 m from the 85 MW research reactor with pure U235 core. The segmented 4 ton Li6-doped liquid scintillator is operated with about 1 m water equivalent overburden and recorded 25461+-283 IBD events. No indication of oscillations into sterile neutrinos was observed. The stated limit for sin**2(2theta(14)) is for Deltam(41)**2 ~ 2 eV**2 where the sensitivity is maximal.


pdgid: S067NUS
text:
AARTSEN 2017B uses three years of upward-going atmospheric neutrino data in the energy range of 10-60 GeV to constrain their disappearance into light sterile neutrinos. The reported limit sin**2(theta)(24) < 0.11 at 90% C.L. is for Deltam**2(41) = 1.0 eV**2. We convert the result to sin**2(2theta)(24) for the listing. AARTSEN 2017B also reports cos**2(theta)(24).sin**2(theta)(34) < 0.15 at 90% C.L. for Deltam**2(41) = 1.0 eV**2.


pdgid: S067NUS
text:
ABDURASHITOV 2017 use the Troitsk nu-mass experiment to search for sterile neutrinos with mass 0.1 - 2 keV. We convert the reported limit from U(e4)**2<0.002 to sin**2(2theta)(14)<0.008 assume U(e4)~ sin(theta)(14). The stated limit corresponds to the smallest U(e4)**2. The exclusion curve begins at U(e4)**2 of 0.02 for m(4) = 0.1 keV.


pdgid: S067NUS
text:
KO 2017 reports on short baseline reactor oscillation search (nubar_e --> nubar_s), motivated be the so-called "reactor antineutrino anomaly". The experiment is conducted at 23.7 m from the core of unit 5 of the Hanbit Nuclear Power Complex in Korea. the reported limited on sin**2(2theta(41)) for sterile neutrinos was determined using the reactor antineutrino spectrum determined by the Daya Bay experiment for Deltam(14)**2 around 0.55 eV**2 where the sensitivity is maximal. A fraction of the parameter space derived from the "reactor antineutrino anomaly" is excluded by this work. Compared to reactor models an event excess is observed at about 5 MeV, in agreement with other experiments.


pdgid: S067NUS
text:
AARTSEN 2016 use one year of upward-going atmospheric muon neutrino data in the energy range of 320 GeV to 20 TeV to constrain their disappearance into light sterile neutrinos. Sterile neutrinos are expected to produce distinctive zenith distribution for these energies for 0.01 <=Deltam**2<=10 eV**2. The stated limit is for sin**2(2theta)(24) at Deltam**2 around 0.3 eV**2.


pdgid: S067NUS
text:
ADAMSON 2016B combine the results of AN 2016B, ADAMSON 2016C, and Bugey-3 reactor experiments to constrain nu_{{mu}} to nu_{{e}} mixing through oscillations into light sterile neutrinos. The stated limit for sin**2(2theta)(mu e) is at |Deltam(41)**2| = 1.2 eV**2.


pdgid: S067NUS
text:
ADAMSON 2016C use the NuMI beam and exposure of 10.56E20 protons on target to search for the oscillation of nu_{{mu}} dominated beam into light sterile neutrinos with detectors at 1.04 and 735 km. The reported limit sin**2(theta(24)) < 0.022 at 95% C.L. is for |Deltam(41)**2| = 0.5 eV**2. We convert the result to sin**2(2theta(24)) for the listing.


pdgid: S067NUS
text:
AN 2016B utilize 621 days of data to place limits on the nubar_{{e}} disappearance into a light sterile neutrino. The stated limit corresponds to the smallest sin**2(2theta(14)) at |Deltam**2(41)| ~ 3E-2 eV**2 (obtained from Figure 3 in AN 2016B). The exclusion curve begins at |Deltam**2(41)|~1.5E-4 eV**2 and extends to ~0.25 eV**2. The analysis assumes sin**2(2theta(12)) = 0.846+-0.021, Deltam**2(21) = 7.53+-0.18E-5 eV**2, and |Deltam**2(32)| = 2.44+-0.06E-3 eV**2.


pdgid: S067NUS
text:
AMBROSIO 2001 tested the pure 2-flavor nu_mu --> nu_s hypothesis using matter effects which change the shape of the zenith-angle distribution of upward through-going muons. With maximum mixing and Deltam**2around 0.0024 eV**2, the nu_mu --> nu_s oscillation isdisfavored with 99% confidence level with respect to the nu_mu --> nu_tau hypothesis.


pdgid: S067NUS
text:
FUKUDA 2000 tested the pure 2-flavor nu_mu --> nu_s hypothesis using three complementary atmospheric-neutrino data samples. With this hypothesis, zenith-angle distributions are expected to show characteristic behavior due to neutral currents and matter effects. In the Deltam**2 and sin**2(2theta)region preferred by the Super-Kamiokande data, the nu_mu --> nu_s hypothesis isrejected at the 99% confidence level, while the nu_mu --> nu_tauhypothesis consistently fits all of the data sample.


pdgid: S067CPT
text:
DEGOUVEA 2005 obtained this bound at the 3sigma CL from the KamLAND (ARAKI 2005) and solar neutrino data.


pdgid: S067CP2
text:
The quoted result is the single-parameter 90% C.L. interval determined from the 90% C.L. contour in the (Deltam**2, Deltambar**2) plane, which is obtained by minimizing the four parameter log-likelihood function with respect to the other oscillation parameters.


pdgid: S077A00
text:
AAD 2025AF searches for W --> e nu_x with displaced decay nu_x --> e e nu, nu_x --> e mu nu or nu_x --> e pi over the range mass(nu_{{x}}) ~ 0.5 -- 16 GeV. Limits are set for both Dirac and Majorana HNLs, as well as for for case in which the mixing coefficients to all three lepton generations are non-zero.


pdgid: S077A00
text:
DREWES 2025 searches for displaced decays nu_x --> e+ e- nu_e from solar-produced HNLs, mainly via ^8B --> ^8Be e nu_x, over the range mass(nu_{{x}}) ~ 1 -- 16 MeV. Limits are derived using data from the space-based detectors Ulysses and the Solar and Heliospheric Observatory. Limits are set for both Dirac and Majorana HNLs, being slightly stronger for the latter.


pdgid: S077A00
text:
HAYRAPETYAN 2025O searches for W --> e nu_x with displaced decay nu_x --> e j, i.e. with one jet, over the range mass(nu_{{x}}) ~ 1 -- 16.5 GeV. Limits are set for both Dirac and Majorana HNLs, as well as for the e mu j final states in terms of the product of electron and muon-HNL couplings.


pdgid: S077A00
text:
AAD 2024AW search for scattering of same-sign boson pairs into same-sign electron pairs, mediated by a virtual Majorana HNL, in the HNL mass range 50 GeV to 20 TeV. Limits are also set for |V(e x) V(mu x)***|.


pdgid: S077A00
text:
AAD 2024BU search for same-sign electron pairs in semileptonic decays of top quarks via a Majorana HNL, in the HNL mass range 15 -- 75 GeV.


pdgid: S077A00
text:
HAYRAPETYAN 2024AB search for W --> e nu_x --> e e lepton nu_lepton prompt decays assuming coupling to a single SM generation, between 10 -- 1500 GeV. Above mass(nu_{{x}}) > mass(W), sensitivity is greatly reduced by the required virtuality of the HNL. Results are quoted for a mass range below mass(W) and just above mass(W), for Majorana HNLs. Similar (weaker) limits also for Dirac HNLs are presented.


pdgid: S077A00
text:
HAYRAPETYAN 2024S search for W --> e nu_x followed by nu_{{x}} displaced decay in flight to electromagnetic and hadronic showers in the CMS muon chamber, in the mass range mass(nu_{{x}}) ~ 1 -- 3 GeV. Limits are set for both Majorana and Dirac HNLs. This long-lived particle style search results in an exclusion region in the coupling-mass plane whose upper contour is determined by an insufficiently long HNL lifetime to reach the muon chambers, and lower contour by insufficient HNL production. The intersection of these, and thus the extent of the experimental sensitivity, occurs at mass(nu_{{x}}) ~ 3 GeV.


pdgid: S077A00
text:
Reanalysis of BEBC results (cf. COOPER-SARKAR 1985) to update searches for D_s()+- --> nu_x e+-  using a corrected formula for the HNL decay probabilities, additional production channels, and an  improved fit for the charm meson distributions. Assumes a Majorana HNL.


pdgid: S077A00
text:
TUMASYAN 2022AD search for W --> e nu_x, nu_x --> e mu nu_mu and set limits for Dirac and Majorana Heavy Neutral Leptons. The data correspond to an integrated luminosity of 138 fb**-1.


pdgid: S077A00
text:
K+ --> e+ nu_x, with nu_{{x}} decay through U(e x). ABE 2019B also considers bounds on |U(lepton x) U(lepton^' x)| for combinations of lepton flavors in the nu_{{x}} decay final state.


pdgid: S077A00
text:
Searches for a Majorana Heavy Neutral Lepton producing a pi- e+ resonance in the same sign dilepton decay D --> K pi- e+ e+.


pdgid: S077A00
text:
BRYMAN 2019 sets best limits |U(ex)|**2 < 1E-4 -- 2E-7 in the mass range mass(nu_{{x}})~2 -- 55 MeV, respectively, using the precision branching ratio measurement in AGUILAR-AREVALO 2015. See also BRYMAN 2019A.


pdgid: S077A00
text:
PARK 2016 quotes an approximate limit B(B+ --> e+ nu_x) < 3E-6 in the mass range mass(nu_{{x}}) ~ 0.2 -- 1.4 GeV.


pdgid: S077A00
text:
Searches for K or pi --> e+ nu_x, nu_x --> e+ e- nu_e using a beam dump experiment at the 70 GeV Serpukhov proton synchrotron. BARANOV 1993 also considers limits for |U(e x) U(mu x)| from K or pi --> mu+ nu_x, nu_x --> e+ e- nu_e.


pdgid: S077A00
text:
ABLIKIM 2025BC search for D_s()+ --> phi e+ nu_x, nu_x --> pi- e+ in the mass range 0.2 -- 0.8 GeV, and set limits on its branching fraction in the range E-5 -- E-2 at 90% CL, respectively.


pdgid: S077A00
text:
HAYRAPETYAN 2024V searches for W --> e nu_x with displaced decay nu_x --> e j, i.e. with one jet, over the range mass(nu_{{x}}) ~ 2 -- 20 GeV. Limits are set for both Dirac and Majorana HNLs.


pdgid: S077A00
text:
AAD 2023AO search for W --> nu_x e, for both Majorana and Dirac HNL scenarios. Also consider scenarios involving multiflavor mixing, with correspondingly weaker limits.


pdgid: S077A01
text:
AAD 2025AF searches for W --> mu nu_x with displaced decay nu_x --> mu mu nu, nu_x --> e mu nu or nu_x --> mu pi over the range mass(nu_{{x}}) ~ 0.5 -- 16 GeV. Limits are set for both Dirac and Majorana HNLs, as well as for for case in which the mixing coefficients to all three lepton generations are non-zero.


pdgid: S077A01
text:
HAYRAPETYAN 2025O searches for W --> mu nu_x with displaced decay nu_x --> mu j, i.e. with one jet, over the range mass(nu_{{x}}) ~ 1 -- 16.5 GeV. Limits are set for both Dirac and Majorana HNLs, as well as for the e mu j final states in terms of the product of electron and muon-HNL couplings.


pdgid: S077A01
text:
AAD 2024BU search for same-sign muon pairs in semileptonic decays of top quarks via a Majorana HNL, in the HNL mass range 15 -- 75 GeV.


pdgid: S077A01
text:
ABRATENKO 2024 search for K+ --> mu+ nu_x, with nu_x --> nu_mu e+ e- and nu_x --> nu_mu pi0 --> nu_mu gamma gamma in the mass ranges mass(nu_{{x}}) ~ 10 -- 150 MeV and mass(nu_{{x}}) ~ 150 -- 245 MeV, respectively, for the case of a Majorana HNL. The pi0 mode dominates above mass(nu_{{x}}) ~ 150 MeV.


pdgid: S077A01
text:
HAYRAPETYAN 2024AB search for W --> mu nu_x --> mu mu lepton nu_lepton prompt decays assuming coupling to a single SM generation, between 10 -- 1500 GeV. Above mass(nu_{{x}}) > mass(W), sensitivity is greatly reduced by the required virtuality of the HNL. Results are quoted for a mass range below mass(W) and just above mass(W), for Majorana HNLs. Similar (weaker) limits also for Dirac HNLs are presented.


pdgid: S077A01
text:
HAYRAPETYAN 2024AC search for B --> X mu nu_x and B --> mu nu_x followed by displaced nu_x --> mu pi+- decay, where X is an unreconstructed hadronic system, for Majorana HNLs. Also considers mixed flavor scenarios with e mu final state lepton pairs, and presents similar (weaker) limits for Dirac HNLs.


pdgid: S077A01
text:
HAYRAPETYAN 2024S search for W --> mu nu_x followed by nu_{{x}} displaced decay in flight to electromagnetic and hadronic showers in the CMS muon chamber, in the mass range mass(nu_{{x}}) ~ 1 -- 3 GeV. Limits are set for both Majorana and Dirac HNLs. This long-lived particle style search results in an exclusion region in the coupling-mass plane whose upper contour is determined by an insufficiently long HNL lifetime to reach the muon chambers, and lower contour by insufficient HNL production. The intersection of these, and thus the extent of the experimental sensitivity, occurs at mass(nu_{{x}}) ~ 3.5 GeV.


pdgid: S077A01
text:
AAD 2023CE search for Majorana HNLs via vector boson fusion W+- W+- --> mu+- mu+-. Limits set in a mass(nu_{{x}}) mass range from 50 GeV up to 20 TeV, using the Phenomenological Type-I Seesaw model as a benchmark scenario.


pdgid: S077A01
text:
TUMASYAN 2023AC search for Majorana HNLs via vector boson fusion W+- W+- --> mu+- mu+-. Limits set in a mass(nu_{{x}}) mass range from 50 GeV up to 25 TeV.


pdgid: S077A01
text:
ABRATENKO 2022A search for K+ --> mu+ nu_x, with nu_x --> mu-+ pi+-, in the mass range mass(nu_{{x}}) ~ 246 -- 385 MeV. Also considers limits from nu_x --> mu- pi+ only, for the case of a Dirac HNL.


pdgid: S077A01
text:
TUMASYAN 2022AD search for W --> mu nu_x, nu_x --> mu e nu_e and set limits for Dirac and Majorana Heavy Neutral Leptons. The data correspond to an integrated luminosity of 138 fb**-1.


pdgid: S077A01
text:
K+ --> mu+ nu_x, with nu_{{x}} decay through U(mu x). ABE 2019B also considers bounds on |U(lepton x) U(lepton^' x)| for combinations of lepton flavors in the nu_{{x}} decay final state.


pdgid: S077A01
text:
PARK 2016 quotes an approximate limit B(B+ --> mu+ nu_x) < 3E-6 in the mass range mass(nu_{{x}}) ~ 0.2 -- 1.4 GeV.


pdgid: S077A01
text:
Search for Heavy Neutral Leptons produced by neutral current muon neutrino interactions, with nu_x --> mu+ mu- nu_mu.


pdgid: S077A01
text:
HAYRAPETYAN 2024V searches for W --> mu nu_x with displaced decay nu_x --> mu j, i.e. with one jet, over the range mass(nu_{{x}}) ~ 2 -- 20 GeV. Limits are set for both Dirac and Majorana HNLs.


pdgid: S077A01
text:
AAD 2023AO search for W --> nu_x mu, for both Majorana and Dirac HNL scenarios. Also consider scenarios involving multiflavor mixing, with correspondingly weaker limits.


pdgid: S077A01
text:
K+ --> mu+ nu_x, with nu_x --> mu- pi+, in the mass range mass(nu_{{x}}) ~ 260 -- 385 MeV.  ABRATENKO 2020 also considers nu_x --> mu+ pi- for the case of a Majorana HNL.


pdgid: S077A02
text:
AAD 2024BU search for same-sign tau pairs in semileptonic decays of top quarks via a Majorana HNL, in the HNL mass range 15 -- 75 GeV.


pdgid: S077A02
text:
HAYRAPETYAN 2024AB search for W --> tau nu_x --> tau tau lepton nu_lepton prompt decays assuming coupling to a single SM generation, between 10 -- 1500 GeV. Above mass(nu_{{x}}) > mass(W), sensitivity is greatly reduced by the required virtuality of the HNL. Results are quoted for a mass range below mass(W) and just above mass(W), for Majorana HNLs. Similar (weaker) limits also for Dirac HNLs are presented.


pdgid: S077A02
text:
HAYRAPETYAN 2024S search for W --> tau nu_x followed by nu_{{x}} displaced decay in flight to electromagnetic and hadronic showers in the CMS muon chamber, in the mass range mass(nu_{{x}}) ~ 1 -- 2 GeV. Limits are set for both Majorana and Dirac HNLs. This long-lived particle style search results in an exclusion region in the coupling-mass plane whose upper contour is determined by an insufficiently long HNL lifetime to reach the muon chambers, and lower contour by insufficient HNL production. The intersection of these, and thus the extent of the experimental sensitivity, occurs at mass(nu_{{x}}) ~ 2 GeV.


pdgid: S077A02
text:
HAYRAPETYAN 2024V searches for W --> tau nu_x with displaced decay nu_x --> tau j, i.e. with one jet, over the range mass(nu_{{x}}) ~ 3 -- 20 GeV. Limits are set for both Dirac and Majorana HNLs.


pdgid: S077A02
text:
NAYAK 2024 searches for tau --> pi nu_x with displaced decay nu_x --> nu_tau mu+ mu- in the Belle central drift chamber (CDC). This long-lived particle style search results in an exclusion region in the coupling-mass plane whose upper contour is determined by an insufficiently long HNL lifetime to reach the CDC, and lower contour by insufficient HNL production. Limits are set for both Dirac and Majorana HNLs.


pdgid: S077A02
text:
Reanalysis of BEBC results (cf. COOPER-SARKAR 1985) to include searches for D_s()+- --> nu_tau tau+-, tau+- --> nu_x pi+-, nu_x rho+-, or nu_x nu_tau lepton+- via  U(tau x). Assumes a Majorana HNL.


pdgid: S077A02
text:
Reanalysis of CHARM results (cf. ORLOFF 2002) to include searches for nu_x --> nu lepton+ lepton-  decays, and including the production of HNLs from tau decays.


pdgid: S077A02
text:
Search for displaced nu_{{x}} decay signatures. Kinematical suppression of nu_x --> tau X at lower masses leads to rapid loosening of the |U(tau x)| bound compared to that for |U(e x)| and |U(mu x)|.


pdgid: S077A02
text:
Search for tau --> pi nu_x, nu_x --> pi e or pi mu in the range 0.2 -- 1.6 GeV. LIVENTSEV 2023 reports results for the sum Sigma(lepton=e,mu,tau)|U(lepton x)|**2 in a model-dependent context, but which may be roughly reinterpreted as a limit |U(e x) U(tau x)|**2 + |U(mu x) U(tau x)|**2 ~< 5E-9 in either Majorana or Dirac HNL scenarios.


pdgid: S077A02
text:
TUMASYAN 2022H sets limits on an approximately mass-degenerate vector-like lepton SU(2)  doublet coupling to the tau. Some of the reported signal region distributions might be used to  set limits for heavy neutral leptons coupled to the tau. The data correspond to an integrated luminosity of 138 fb**-1.


pdgid: Q123UM
text:
DOMINGUEZ 2019 determine the quark mass from a QCD finite energy sum rule for the divergence of the axial current.


pdgid: Q123UM
text:
BAZAVOV 2018 determine the quark masses using a lattice computation with staggered fermions and four active quark flavors.


pdgid: Q123UM
text:
FODOR 2016 is a lattice simulation with n_{{f}} = 2 + 1 dynamical flavors and includes partially quenched QED effects.


pdgid: Q123UM
text:
CARRASCO 2014 is a lattice QCD computation of light quark masses using 2 + 1 + 1 dynamical quarks, with m_{{u}} = m_{{d}} not= m_{{s}} not= m_{{c}}. The u and d quark masses are obtained separately by using the K meson mass splittings and lattice results for the electromagnetic contributions.


pdgid: Q123UM
text:
BLUM 2010 determines light quark masses using a QCD plus QED lattice computation of the electromagnetic mass splittings of the low-lying hadrons. The lattice simulations use 2+1 dynamical quark flavors.


pdgid: Q123UM
text:
DAVIES 2010 and MCNEILE 2010 determine mbar_{{c}}(mu)/mbar_{{s}}(mu) = 11.85+-0.16 using a lattice computation with n_{{f}} = 2 + 1 dynamical fermions of the pseudoscalar meson masses. Mass mass(u) is obtained from this using the value of mass(c) from ALLISON 2008 or MCNEILE 2010 and the BAZAVOV 2010 values for the light quark mass ratios, mass(s)/mbar and mass(u)/mass(d).


pdgid: Q123UM
text:
DURR 2011 determine quark mass from a lattice computation of the meson spectrum using n_{{f}} = 2 + 1 dynamical flavors. The lattice simulations were done at the physical quark mass, so that extrapolation in the quark mass was not needed. The individual mass(u), mass(d) values are obtained using the lattice determination of the average mass mass(ud) and of the ratio mass(s)/mass(ud) and the value of Q = (mass**2(s) - mass**2(ud)) / (mass**2(d) - mass**2(u)) as determined from eta --> 3pi decays.


pdgid: Q123UM
text:
DOMINGUEZ 2009 use QCD finite energy sum rules for the two-point function of the divergence of the axial vector current computed to order alpha(s)**4.


pdgid: Q123UM
text:
DEANDREA 2008 determine mass(u)-mass(d) from eta --> 3pi0, and combine with the PDG 2006 lattice average value of mass(u)+mass(d) = 7.6+-1.6 to determine mass(u) and mass(d).


pdgid: Q123UM
text:
BLUM 2007 determine quark masses from the pseudoscalar meson masses using a QED plus QCD lattice computation with two dynamical quark flavors.


pdgid: Q123UM
text:
JAMIN 2006 determine mass(u)(2 GeV) by combining the value of mass(s) obtained from the spectral function for the scalar K pi form factor with other determinations of the quark mass ratios.


pdgid: Q123UM
text:
MASON 2006 extract light quark masses from a lattice simulation using staggered fermions with an improved action, and three dynamical light quark flavors with degenerate u and d quarks. Perturbative corrections were included at NNLO order. The quark masses mass(u) and mass(d) were determined from their (mass(u)+mass(d))/2 measurement and AUBIN 2004A mass(u)/mass(d) value.


pdgid: Q123UM
text:
NARISON 2006 uses sum rules for e+ e- --> hadrons to order alpha_{{s}}^3() to determine mass(s) combined with other determinations of the quark mass ratios.


pdgid: Q123DM
text:
DAVIES 2010 and MCNEILE 2010 determine mbar_{{c}}(mu)/mbar_{{s}}(mu) = 11.85+-0.16 using a lattice computation with n_{{f}} = 2 + 1 dynamical fermions of the pseudoscalar meson masses. Mass mass(d) is obtained from this using the value of mass(c) from ALLISON 2008 or MCNEILE 2010 and the BAZAVOV 2010 values for the light quark mass ratios, mass(s)/mbar and mass(u)/mass(d).


pdgid: Q123DM
text:
JAMIN 2006 determine mass(d)(2 GeV) by combining the value of mass(s) obtained from the spectral function for the scalar K pi form factor with other determinations of the quark mass ratios.


pdgid: Q123DM
text:
AUBIN 2004A perform three flavor dynamical lattice calculation of pseudoscalar meson masses, with continuum estimate of electromagnetic effects in the kaon masses, and one-loop perturbative renormalization constant.


pdgid: Q123MR4
text:
ALEXANDROU 2021 determines the quark mass using a lattice calculation of the meson and baryon  masses with a twisted mass fermion action. The simulations are carried out using 2+1+1 dynamical  quarks with mass(u) = mass(d)not=mass(s)not=mass(c), including gauge ensembles  close to the physical pion point.


pdgid: Q123MR4
text:
BRUNO 2020 determines the light quark mass using a lattice calculation with n_{{f}} = 2+1  flavors of Wilson fermions. The scale has been set from f_{{pi}} and f_{{K}}. The tuning was done  using the masses of the lightest (pi) and strange (K) pseudoscalar mesons.


pdgid: Q123MR4
text:
YUAN 2017 determine mbar using QCD sum rules in the isospin I=0 scalar channel. At the end of the "Numerical Results" section of YUAN 2017 the authors discuss the significance of their larger value of the light quark mass compared to previous determinations.


pdgid: Q123MR4
text:
ARTHUR 2013 is a lattice computation using 2+1 dynamical domain wall fermions. Masses at mu = 3 GeV have been converted to mu = 2 GeV using conversion factors given in their paper.


pdgid: Q123MR4
text:
DURR 2011 determine quark mass from a lattice computation of the meson spectrum using n_{{f}} = 2 + 1 dynamical flavors. The lattice simulations were done at the physical quark mass, so that extrapolation in the quark mass was not needed.


pdgid: Q123MR4
text:
BLOSSIER 2010 determines quark masses from a computation of the hadron spectrum using n_{{f}}=2 dynamical twisted-mass Wilson fermions.


pdgid: Q123MR4
text:
DAVIES 2010 and MCNEILE 2010 determine mbar_{{c}}(mu)/mbar_{{s}}(mu) = 11.85+-0.16 using a lattice computation with n_{{f}} = 2 + 1 dynamical fermions of the pseudoscalar meson masses. Mass mbar is obtained from this using the value of mass(c) from ALLISON 2008 or MCNEILE 2010 and the BAZAVOV 2010 values for the light quark mass ratio, mass(s)/mbar.


pdgid: Q123MR4
text:
AOKI 2011A determine quark masses from a lattice computation of the hadron spectrum using n_{{f}} = 2 + 1 dynamical flavors of domain wall fermions.


pdgid: Q123MR4
text:
ALLTON 2008 use a lattice computation of the pi, K, and Omega masses with 2+1 dynamical flavors of domain wall quarks, and non-perturbative renormalization.


pdgid: Q123MR4
text:
BLOSSIER 2008 use a lattice computation of pseudoscalar meson masses and decay constants with 2 dynamical flavors and non-perturbative renormalization.


pdgid: Q123MR4
text:
ISHIKAWA 2008 use a lattice computation of the light meson spectrum with 2+1 dynamical flavors of O(a) improved Wilson quarks, and one-loop perturbative renormalization.


pdgid: Q123MR4
text:
NAKAMURA 2008 do a lattice computation using quenched domain wall fermions and non-perturbative renormalization.


pdgid: Q123MR4
text:
GOCKELER 2006 use an unquenched lattice computation of the axial Ward Identity with n_{{f}} = 2 dynamical light quark flavors, and non-perturbative renormalization, to obtain mbar(2 GeV) = 4.08+-0.25+-0.19+-0.23 MeV, where the first error is statistical, the second and third are systematic due to the fit range and force scale uncertainties, respectively. We have combined the systematic errors linearly.


pdgid: Q123MR4
text:
GOCKELER 2006A use an unquenched lattice computation of the pseudoscalar meson masses with n_{{f}} = 2 dynamical light quark flavors, and non-perturbative renormalization.


pdgid: Q123MR4
text:
MASON 2006 extract light quark masses from a lattice simulation using staggered fermions with an improved action, and three dynamical light quark flavors with degenerate u and d quarks. Perturbative corrections were included at NNLO order.


pdgid: Q123MR4
text:
AUBIN 2004 perform three flavor dynamical lattice calculation of pseudoscalar meson masses, with one-loop perturbative renormalization constant.


pdgid: Q123MR4
text:
AOKI 2003 uses quenched lattice simulation of the meson and baryon masses with degenerate light quarks. The extrapolations are done using quenched chiral perturbation theory.


pdgid: Q123MR4
text:
The errors given in AOKI 2003B were +0.046. We changed them to +-0.3 for calculating the overall best values. AOKI 2003B uses lattice simulation of the meson and baryon masses with two dynamical light quarks. Simulations are performed using the O(a) improved Wilson action.


pdgid: Q123MR4
text:
BECIREVIC 2003 perform quenched lattice computation using the vector and axial Ward identities. Uses O(a) improved Wilson action and nonperturbative renormalization.


pdgid: Q123MR4
text:
CHIU 2003 determines quark masses from the pion and kaon masses using a lattice simulation with a chiral fermion action in quenched approximation.


pdgid: Q123MR0
text:
AUBIN 2004A perform three flavor dynamical lattice calculation of pseudoscalar meson masses, with continuum estimate of electromagnetic effects in the kaon masses.


pdgid: Q123MR0
text:
NELSON 2003 computes coefficients in the order p**4 chiral Lagrangian using a lattice calculation with three dynamical flavors. The ratio mass(u)/mass(d) is obtained by combining this with the chiral perturbation theory computation of the meson masses to order p**4.


pdgid: Q123MR0
text:
LEUTWYLER 1996 uses a combined fit to eta --> 3pi and psi^' --> J/psi (pi,eta) decay rates, and the electromagnetic mass differences of the pi and K.


pdgid: Q123SM
text:
COLQUHOUN 2026 value comes from lattice computation of the pseudoscalar correlator. Quenched QED corrections are included.


pdgid: Q123SM
text:
BRUNO 2020 determines the light quark mass using a lattice calculation with n_{{f}} = 2+1 flavors of Wilson fermions. The scale has been set from f_{{pi}} and f_{{K}}. The tuning was done using the masses of the lightest (pi) and strange (K) pseudoscalar mesons.


pdgid: Q123SM
text:
LYTLE 2018 combined with CHAKRABORTY 2015 determine mbar_{{s}}(3 GeV) = 84.78+-0.65 MeV from a lattice simulation with n_{{f}} = 2+1+1 flavors. They also determine the quoted value mbar_{{s}}(2 GeV) for n_{{f}} = 4 dynamical flavors.


pdgid: Q123SM
text:
ANANTHANARAYAN 2016 determine mbar_{{s}}(2 GeV) = 106.70+-9.36 MeV and 74.47+-7.77 MeV from fits to ALEPH and OPAL tau decay data, respectively. We have used the weighted average of the two.


pdgid: Q123SM
text:
BODENSTEIN 2013 determines mass(s) from QCD finite energy sum rules, and the perturbative computation of the pseudoscalar correlator to five-loop order.


pdgid: Q123SM
text:
CHAKRABORTY 2015 is a lattice QCD computation that determines mass(c) and mass(c)/mass(s) using pseudoscalar mesons masses tuned on gluon field configurations with 2+1+1 dynamical flavors of HISQ quarks with u/d masses down to the physical value.


pdgid: Q123SM
text:
DAVIES 2010 and MCNEILE 2010 determine mbar_{{c}}(mu)/mbar_{{s}}(mu) = 11.85+-0.16 using a lattice computation with n_{{f}} = 2 + 1 dynamical fermions of the pseudoscalar meson masses. Mass mass(s) is obtained from this using the value of mass(c) from ALLISON 2008 or MCNEILE 2010.


pdgid: Q123SM
text:
DOMINGUEZ 2008A make determination from QCD finite energy sum rules for the pseudoscalar two-point function computed to order alpha(s)**4.


pdgid: Q123SM
text:
GOCKELER 2006 use an unquenched lattice computation of the axial Ward Identity with n_{{f}} = 2 dynamical light quark flavors, and non-perturbative renormalization, to obtain mbar_{{s}}(2 GeV) = 111+-6+-4+-6 MeV, where the first error is statistical, the second and third are systematic due to the fit range and force scale uncertainties, respectively. We have combined the systematic errors linearly.


pdgid: Q123SM
text:
BAIKOV 2005 determines mbar_{{s}}(M_{{tau}}) = 100+5-3+17-19 from sum rules using the strange spectral function in tau decay. The computations were done to order alpha_{{s}}^3(), with an estimate of the alpha_{{s}}^4() terms. We have converted the result to mu = 2 GeV.


pdgid: Q123SM
text:
GAMIZ 2005 determines mbar_{{s}}(2 GeV) from sum rules using the strange spectral function in tau decay. The computations were done to order alpha_{{s}}^2(), with an estimate of the alpha_{{s}}^3() terms.


pdgid: Q123SM
text:
NARISON 2005 determines mbar_{{s}}(2 GeV) from sum rules using the strange spectral function in tau decay. The computations were done to order alpha_{{s}}^3().


pdgid: Q123SM
text:
AOKI 2003 uses quenched lattice simulation of the meson and baryon masses with degenerate light quarks. The extrapolations are done using quenched chiral perturbation theory. Determines m(s)=113.8+-2.3+5.8-2.9 using K mass as input and m(s)=142.3+-5.8+22-0 using phi mass as input. We have performed a weighted average of these values.


pdgid: Q123SM
text:
AOKI 2003B uses lattice simulation of the meson and baryon masses with two dynamical light quarks. Simulations are performed using the O(a) improved Wilson action.


pdgid: Q123SM
text:
BECIREVIC 2003 perform quenched lattice computation using the vector and axial Ward identities. Uses O(a) improved Wilson action and nonperturbative renormalization. They also quote mbar/m(s)=24.3+-0.2+-0.6.


pdgid: Q123SM
text:
GAMIZ 2003 determines mass(s) from SU(3) breaking in the tau hadronic width. The value of V(u s) is chosen to satisfy CKM unitarity.


pdgid: Q123SM
text:
GAMIZ 2003 determines mass(s) from SU(3) breaking in the tau hadronic width. The value of V(u s) is taken from the PDG.


pdgid: Q123MR1
text:
DONOGHUE 1992 result is from a combined analysis of meson masses, eta --> 3pi using second-order chiral perturbation theory including nonanalytic terms, and (psi(2S) --> J/psi(1S) pi)/(psi(2S) --> J/psi(1S) eta).


pdgid: Q123MR1
text:
LEUTWYLER 1990B determines quark mass ratios using second-order chiral perturbation theory for the meson and baryon masses, including nonanalytic corrections. Also uses Weinberg sum rules to determine L(7).


pdgid: Q123MR3
text:
COLANGELO 2017 obtain Q from a dispersive analysis of KLOE collaboration data on eta --> pi+ pi- pi0 decays and chiral perturbation theory input.


pdgid: Q123MR3
text:
GUO 2017 determine Q from a dispersive model fit to KLOE and WASA-at-COSY data on eta --> pi+ pi- pi0 decay and matching to chiral perturbation theory.


pdgid: Q123MR3
text:
ANISOVICH 1996 find Q from eta --> pi+ pi- pi0 decay using dispersion relations and chiral perturbation theory.


pdgid: Q004M
text:
ALEXANDROU 2021 determines the quark mass using a lattice calculation of the meson and baryon   masses with a twisted mass fermion action. We have converted mbar_{{c}}(3 GeV) = 1.036+-0.017+0.015-0.008 to   mbar_{{c}}(mbar_{{c}}). The simulations are carried out using 2+1+1 dynamical quarks with  mass(u) = mass(d)not=mass(s)not=mass(c), including gauge ensembles close to the  physical pion point.


pdgid: Q004M
text:
HEITGER 2021 determines the charm quark mass using a n_{{f}} = 2+1 flavor lattice QCD  simulation with non-perturbatively O(a) improved Wilson fermions. They also determine mbar_{{c}}(3  GeV) = 1.007+-0.016 GeV.


pdgid: Q004M
text:
HATTON 2020 determines the charm quark mass with a lattice QCD + quenched QED simulation using the HISQ action and including n_{{f}} = 2+1+1 flavors of sea quarks. mass(c) is tuned from the J/psi meson mass giving mbar_{{c}}(3 GeV) = 0.9841+-0.0051 GeV.


pdgid: Q004M
text:
NARISON 2020 determines the quark mass using QCD Laplace sum rules from the B_{{c}} mass, combined with previous determinations of the QCD condensates and c and b masses.


pdgid: Q004M
text:
ABRAMOWICZ 2018 determine mbar_{{c}}(mbar_{{c}}) = 1.290+0.046-0.041+0.062-0.014+0.003-0.031 from the production of c quarks in e p collisions at HERA using combined H1 and ZEUS data. The experimental/fitting errors, and those from modeling and parameterization have been combined in quadrature.


pdgid: Q004M
text:
LYTLE 2018 combined with CHAKRABORTY 15 determine mbar_{{c}}(3 GeV) = 0.9874(48) GeV from a lattice simulation with n_{{f}} = 2+1+1 flavors. They also determine the quoted value mbar_{{c}}(mbar_{{c}}) for n_{{f}} = 4 dynamical flavors.


pdgid: Q004M
text:
PESET 2018 determine mbar_{{c}}(mbar_{{c}}) and mbar_{{b}}(mbar_{{b}}) using an N3LO calculation of the eta_{{c}}, eta_{{b}} and B_{{c}} masses.


pdgid: Q004M
text:
CHETYRKIN 2017 determine mbar_{{c}}(mu = 3 GeV) = 0.993+-0.008 GeV and mbar_{{c}}(mbar_{{c}}) from a four-loop sum-rule computation of the cross-section for e+ e- --> hadrons in the charm threshold region.


pdgid: Q004M
text:
ERLER 2017 determine mbar_{{c}}(mbar_{{c}}) = 1.272+-0.008 GeV from a three-loop QCD sum-rule computation of the vector current correlator. This result is for fixed alpha_{{s}}(M(Z)) = 0.1182. Including an alpha_{{s}} uncertainty of +-0.0016, the charm mass error increases from 8 to 9 MeV.


pdgid: Q004M
text:
DEHNADI 2015 determine mbar_{{c}}(mbar_{{c}}) using sum rules for e+ e- --> hadrons at order alpha_{{s}}^3() (N3LO), and fitting to both experimental data and lattice results.


pdgid: Q004M
text:
ALEKHIN 2013 determines mass(c) from charm production in deep inelastic scattering at HERA using approximate NNLO QCD.


pdgid: Q004M
text:
SAMOYLOV 2013 determines mass(c) from a study of charm dimuon production in neutrino-iron scattering using the NLO QCD result for the charm quark production cross section.


pdgid: Q004M
text:
BODENSTEIN 2011 determine mbar_{{c}}(3 GeV) = 0.987+-0.009 GeV and mbar_{{c}}(mbar_{{c}}) = 1.278+-0.009 GeV using QCD sum rules for the charm quark vector current correlator.


pdgid: Q004M
text:
LASCHKA 2011 determine the c mass from the charmonium spectrum. The theoretical computation uses the heavy potential to order 1/mass(Q) obtained by matching the short-distance perturbative result onto lattice QCD result at larger scales.


pdgid: Q004M
text:
AUBERT 2010A determine the b- and c-quark masses from a fit to the inclusive decay spectra in semileptonic B decays in the kinetic scheme (and convert it to the MSbar scheme).


pdgid: Q004M
text:
SIGNER 2009 determines the c-quark mass using non-relativistic sum rules to analyze the e+ e- --> c cbar cross-section near threshold. Also determine the PS mass (mu(F)= 0.7 GeV) = 1.50+-0.04 GeV.


pdgid: Q004M
text:
NARISON 2018A determines simultaneously mbar_{{c}}(mbar_{{c}}) and the 4-dimension gluon condensate using QCD exponential sum rules and their ratios evaluated at the optimal scale mu = 2.85 GeV at N2LO-N3LO of perturbative QCD and including condensates up to dimension 6 -- 8 in the (axial-)vector and (pseudo-)scalar charmonium channels.


pdgid: Q004M
text:
NARISON 2018B determines mbar_{{c}}(mbar_{{c}}) using QCD vector moment sum rules and their ratios at N2LO-N3LO of perturbative QCD and including condensates up to dimension 8.


pdgid: Q004M
text:
BERTONE 2016 determine mbar_{{c}}(mbar_{{c}}) from HERA deep inelastic scattering data using the FONLL scheme. Also determine mbar_{{c}}(mbar_{{c}})=1.318+-0.054+0.490-0.022 using the fixed flavor number scheme.


pdgid: Q004M
text:
CHAKRABORTY 2015 is a lattice QCD computation using 2+1+1 dynamical flavors. Moments of pseudoscalar current-current correlators are matched to alpha_{{s}}^3()-accurate QCD perturbation theory with the eta_{{c}} meson mass tuned to experiment.


pdgid: Q004M
text:
ABRAMOWICZ 2013C determines mass(c) from charm production in deep inelastic e p scattering, using the QCD prediction at NLO order. The uncertainties from model and parameterization assumptions, and the value of alpha_{{s}}, of +-0.03, +- 0.02, and +- 0.02 respectively, have been combined in quadrature.


pdgid: Q004M
text:
DEHNADI 2013 determines mass(c) using QCD sum rules for the charmonium spectrum and charm continuum to order alpha_{{s}}^3 (N3LO). The statistical and systematic experimental errors of +-0.006 and +-0.009 have been combined in quadrature. The theoretical uncertainties +-0.019 from truncation of the perturbation series, +-0.010 from alpha_{{s}}, and +-0.002 from the gluon condensate have been combined in quadrature.


pdgid: Q004M
text:
NARISON 2013 determines mass(c) using QCD spectral sum rules to order alpha_{{s}}^2 (NNLO) and including condensates up to dimension 6.


pdgid: Q004M
text:
ALEKHIN 2012 determines mass(c) from heavy quark production in deep inelastic scattering at HERA using approximate NNLO QCD.


pdgid: Q004M
text:
NARISON 2012A determines mass(c) using sum rules for the vector current correlator to order alpha_{{s}}^3(), including the effect of gluon condensates up to dimension eight.


pdgid: Q004M
text:
ALEKHIN 2011 determines mass(c) from heavy quark production in deep inelastic scattering using fixed target and HERA data, and approximate NNLO QCD.


pdgid: Q004M
text:
BODENSTEIN 2010 determines mbar_{{c}}(3 GeV) = 1.008+-0.026 GeV using finite energy sum rules for the vector current correlator. The authors have converted this to mbar_{{c}}(mbar_{{c}}) using alpha_{{s}}(M_{{Z}}) = 0.1189+-0.0020.


pdgid: Q004M
text:
MCNEILE 2010 determines mass(c) by comparing the order alpha_{{s}}^3 perturbative results for the pseudo-scalar current to lattice simulations with n_{{f}} = 2+1 sea-quarks by the HPQCD collaboration.


pdgid: Q004M
text:
NARISON 2010 determines mass(c) from ratios of moments of vector current correlators computed to order alpha_{{s}}^3() and including the dimension-six gluon condensate.


pdgid: Q004M
text:
CHETYRKIN 2009 determine mass(c) and mass(b) from the e+ e- --> Q Qbar cross-section and sum rules, using an order alpha_{{s}}^3 computation of the heavy quark vacuum polarization. They also determine mass(c)(3 GeV) = 0.986+-0.013GeV.


pdgid: Q004M
text:
ALLISON 2008 determine mass(c) by comparing four-loop perturbative results for the pseudo-scalar current correlator to lattice simulations by the HPQCD collaboration. The result has been updated in MCNEILE 2010.


pdgid: Q004M
text:
KUHN 2007 determine mbar_{{c}}(mu = 3 GeV) = 0.986+-0.013 GeV and mbar_{{c}}(mbar_{{c}}) from a four-loop sum-rule computation of the cross-section for e+ e- --> hadrons in the charm threshold region.


pdgid: Q004M
text:
BOUGHEZAL 2006 result comes from the first moment of the hadronic production cross-section to order alpha_{{s}}^3().


pdgid: Q004M
text:
HOANG 2006 determines mbar_{{c}}(mbar_{{c}}) from a global fit to inclusive B decay data. The B decay distributions were computed to order alpha_{{s}}^2()beta_{{0}}(), and the conversion between different m_{{c}} mass schemes to order alpha_{{s}}^3().


pdgid: Q004M
text:
AUBERT 2004X obtain mass(c) from a fit to the hadron mass and lepton energy distributions in semileptonic B decay. The paper quotes values in the kinetic scheme. The MSbar value has been provided by the BABAR collaboration.


pdgid: Q004M
text:
HOANG 2004 determines mbar_{{c}}(mbar_{{c}}) from moments at order alpha_{{s}}^2() of the charm production cross-section in e+ e- annihilation.


pdgid: Q004M
text:
ZYABLYUK 2003 determines m(c) by using QCD sum rules in the pseudoscalar channel and comparing with the eta(c) mass.


pdgid: Q004MSR
text:
CHAKRABORTY 2015 is a lattice QCD computation on gluon field configurations with 2+1+1 dynamical flavors of HISQ quarks with u/d masses down to the physical value. mass(c) and mass(s) are tuned from pseudoscalar meson masses.


pdgid: Q004MSR
text:
DURR 2012 determine mass(c)/mass(s) using a lattice computation with n_{{f}} = 2 dynamical fermions. The result is combined with other determinations of mass(c) to obtain mass(s)(2 GeV) = 97.0+-2.6+-2.5 MeV.


pdgid: Q004MSR
text:
DAVIES 2010 determine mass(c)/mass(s) from meson masses calculated on gluon fields including u, d, and s sea quarks with lattice spacing down to 0.045 fm. The Highly Improved Staggered quark formalism is used for the valence quarks.


pdgid: Q004MSR
text:
BLOSSIER 2010 determine mass(c)/mass(s) from a computation of the hadron spectrum using n_{{f}} = 2 dynamical twisted-mass Wilson fermions.


pdgid: Q004MBR
text:
HATTON 2021 determine mbar_{{b}}(mu)/mbar_{{c}}(mu) = 4.586+-0.012 at mu = 3  GeV with a lattice QCD + quenched QED simulation using the HISQ action and including n_{{f}} =2+1+1 flavors of sea quarks. The ratio depends weakly on mu because of QED effects.


pdgid: Q004MBR
text:
BAZAVOV 2018 determine the quark masses using a lattice computation with staggered fermions and four active quark flavors for the u, d, s, c quarks and five active flavors for the b quark.


pdgid: Q004MDB
text:
AUBERT 2010A determine the b- and c-quark masses from a fit to the inclusive decay spectra in semileptonic B decays in the kinetic scheme.


pdgid: Q004MDB
text:
ABDALLAH 2006B determine mass(b)-mass(c) from moments of the hadron invariant mass and lepton energy spectra in semileptonic inclusive B decays.


pdgid: Q005M
text:
APARISI 2022 determine m_{{b}} at the Higgs mass, mbar_{{b}}(m_{{H}}) = 2.60+0.36-0.31 GeV from Higgs boson decay rates at the LHC, which is used to obtain mbar_{{b}}(mbar_{{b}}).


pdgid: Q005M
text:
HATTON 2021 determine mbar_{{b}}(3 GeV) = 4.513+-0.026 GeV using a lattice QCD + quenched QED simulation using the HISQ action and including n_{{f}} = 2+1+1 flavors of sea quarks, by combining their mbar_{{b}}/mbar_{{c}} and mbar_{{c}} determinations.


pdgid: Q005M
text:
ABRAMOWICZ 2018 determine mbar_{{b}}(mbar_{{b}}) = 4.049+0.104-0.109+0.090-0.032+0.001-0.031 from the production of b quarks in e p collisions at HERA using combined H1 and ZEUS data. The experimental/fitting errors, and those from modeling and parameterization have been combined in quadrature.


pdgid: Q005M
text:
BAZAVOV 2018 determine the b mass using a lattice computation with staggered fermions and five active quark flavors.


pdgid: Q005M
text:
KIYO 2016 determine mbar_{{b}}(mbar_{{b}}) from the Upsilon(1S) mass at order alpha_{{s}}^3() (N3LO).


pdgid: Q005M
text:
ALBERTI 2015 determine mbar_{{b}}(mbar_{{b}}) from fits to inclusive B --> X_c e nubar decay. They also find m(b)**kin(1 GeV) = 4.553+-0.020 GeV.


pdgid: Q005M
text:
BENEKE 2015 determine mbar_{{b}}(mbar_{{b}}) using sum rules for e+ e- --> hadrons at order N3LO including finite mass(c) effects. They find m(b)**PS(2 GeV) = 4.532+0.013-0.039 GeV, and mbar_{{b}}(mbar_{{b}}) = 4.193+0.022-0.035 GeV. The value quoted is obtained using the four-loop conversion given in BENEKE 2016.


pdgid: Q005M
text:
COLQUHOUN 2015 determine mbar_{{b}}(mbar_{{b}}) from moments of the vector current correlator computed with a lattice simulation using the NRQCD action.


pdgid: Q005M
text:
DEHNADI 2015 determine mbar_{{b}}(mbar_{{b}}) using sum rules for e+ e- --> hadrons at order alpha_{{s}}^3() (N3LO), and fitting to both experimental data and lattice results.


pdgid: Q005M
text:
BERNARDONI 2014 determine m_{{b}} from n_{{f}} = 2 lattice calculations using heavy quark effective theory non-perturbatively renormalized and matched to QCD at 1/m order.


pdgid: Q005M
text:
PENIN 2014 determine mbar_{{b}}(mbar_{{b}}) = 4.169+-0.008+-0.002+-0.002 using an estimate of the order alpha_{{s}}^3() b-quark vacuum polarization function in the threshold region, including finite mass(c) effects. The errors of +-0.008 from theoretical uncertainties, and +-0.002 from alpha_{{s}} have been combined in quadrature.


pdgid: Q005M
text:
LEE 2013O determines mass(b) using lattice calculations of the Upsilon and B_{{s}} binding energies in NRQCD, including three light dynamical quark flavors. The quark mass shift in NRQCD is determined to order alpha_{{s}}^2(), with partial alpha_{{s}}^3() contributions.


pdgid: Q005M
text:
LUCHA 2013 determines mass(b) from QCD sum rules for heavy-light currents using the lattice value for f_{{B}} of 191.5+-7.3 GeV.


pdgid: Q005M
text:
BODENSTEIN 2012 determine mass(b) using sum rules for the vector current correlator and the e+ e- --> Q Qbar total cross-section.


pdgid: Q005M
text:
DIMOPOULOS 2012 determine quark masses from a lattice computation using n_{{f}} = 2 dynamical flavors of twisted mass fermions.


pdgid: Q005M
text:
LASCHKA 2011 determine the b mass from the charmonium spectrum. The theoretical computation uses the heavy potential to order 1/mass(Q) obtained by matching the short-distance perturbative result onto lattice QCD result at larger scales.


pdgid: Q005M
text:
CHETYRKIN 2009 determine mass(c) and mass(b) from the e+ e- --> Q Qbar cross-section and sum rules, using an order alpha_{{s}}^3 (N3LO) computation of the heavy quark vacuum polarization.


pdgid: Q005M
text:
SCHWANDA 2008 measure moments of the inclusive photon spectrum in B --> X_s gamma decay to determine m_{{b}}^1S(). We have converted this to MSbar scheme.


pdgid: Q005M
text:
NARISON 2018A determines mbar_{{b}}(mbar_{{b}}) as a function of alpha_{{s}} using QCD exponential sum rules and their ratios evaluated at the optimal scale mu = 9.5 GeV at N2LO-N3LO of perturbative QCD and including condensates up to dimension 6 -- 8 in the (axial-)vector and (pseudo-)scalar bottomonium channels.


pdgid: Q005M
text:
NARISON 2018B determines mbar_{{b}}(mbar_{{b}}) using QCD vector moment sum rules and their ratios at N2LO-N3LO of perturbative QCD and including condensates up to dimension 8.


pdgid: Q005M
text:
ABRAMOWICZ 2014A determine mbar_{{b}}(mbar_{{b}}) = 4.07+-0.14+0.01-0.07+0.05-0.00+0.08-0.05 from the production of b quarks in e p collisions at HERA. The errors due to fitting, modeling, PDF parameterization, and theoretical QCD uncertainties due to the values of alpha_{{s}}, m_{{c}}, and the renormalization scale mu have been combined in quadrature.


pdgid: Q005M
text:
AYALA 2014A determine mbar_{{b}}(mbar_{{b}}) from the Upsilon(1S) mass computed to N3LO order in perturbation theory using a renormalon subtracted scheme.


pdgid: Q005M
text:
NARISON 2013 determines mass(b) using QCD spectral sum rules to order alpha_{{s}}^2 (NNLO) and including condensates up to dimension 6.


pdgid: Q005M
text:
NARISON 2013A determines mass(b) using HQET sum rules to order alpha_{{s}}^2 (NNLO) and the B meson mass and decay constant.


pdgid: Q005M
text:
HOANG 2012 determine mass(b) using non-relativistic sum rules for the Upsilon system at order alpha_{{s}}^2 (NNLO) with renormalization group improvement.


pdgid: Q005M
text:
NARISON 2012 determines mass(b) using exponential sum rules for the vector current correlator to order alpha_{{s}}^3(), including the effect of gluon condensates up to dimension eight.


pdgid: Q005M
text:
Determines mass(b) to order alpha_{{s}}^3() (N3LO), including the effect of gluon condensates up to dimension eight combining the methods of NARISON 2012 and NARISON 2012A.


pdgid: Q005M
text:
NARISON 2012A determines mass(b) using sum rules for the vector current correlator to order alpha_{{s}}^3(), including the effect of gluon condensates up to dimension eight.


pdgid: Q005M
text:
MCNEILE 2010 determines mass(b) by comparing order alpha_{{s}}^3 (N3LO) perturbative results for the pseudo-scalar current to lattice simulations with n_{{f}} = 2+1 sea-quarks by the HPQCD collaboration.


pdgid: Q005M
text:
NARISON 2010 determines mass(b) from ratios of moments of vector current correlators computed to order alpha_{{s}}^3() and including the dimension-six gluon condensate. These values are taken from the erratum to that reference.


pdgid: Q005M
text:
ABDALLAH 2008D determine mbar_{{b}}(M_{{Z}}) = 3.76+-1.0 GeV from a leading order study of four-jet rates at LEP.


pdgid: Q005M
text:
GUAZZINI 2008 determine mbar_{{b}}(mbar_{{b}}) from a quenched lattice simulation of heavy meson masses. The +-0.08 is an estimate of the quenching error.


pdgid: Q005M
text:
DELLA-MORTE 2007 determine mbar_{{b}}(mbar_{{b}}) from a computation of the spin-averaged B meson mass using quenched lattice HQET at order 1/m. The +-0.08 is an estimate of the quenching error.


pdgid: Q005M
text:
KUHN 2007 determine mbar_{{b}}(mu = 10 GeV) = 3.609+-0.025 GeV and mbar_{{b}}(mbar_{{b}}) from a four-loop sum-rule computation of the cross-section for e+ e- --> hadrons in the bottom threshold region.


pdgid: Q005M
text:
ABDALLAH 2006D determine mass(b)(M_{{Z}}) = 2.85+-0.32 GeV from Z-decay three-jet events containing a b-quark.


pdgid: Q005M
text:
BOUGHEZAL 2006 MSbar scheme result comes from the first moment of the hadronic production cross-section to order alpha_{{s}}^3().


pdgid: Q005M
text:
PINEDA 2006 MSbar scheme result comes from a partial NNLL evaluation (complete at order alpha_{{s}}^2 (NNLO)) of sum rules of the bottom production cross-section in e+ e- annihilation.


pdgid: Q005M
text:
GRAY 2005 determines mbar_{{b}}(mbar_{{b}}) from a lattice computation of the Upsilon spectrum. The simulations have 2+1 dynamical light flavors. The b quark is implemented using NRQCD.


pdgid: Q005M
text:
AUBERT 2004X obtain mass(b) from a fit to the hadron mass and lepton energy distributions in semileptonic B decay. The paper quotes values in the kinetic scheme. The MSbar value has been provided by the BABAR collaboration.


pdgid: Q005M
text:
BAUER 2004 determine mass(b), mass(c) and mass(b)-mass(c) by a global fit to inclusive B decay spectra.


pdgid: Q005M
text:
HOANG 2004 determines mbar_{{b}}(mbar_{{b}}) from moments at order alpha_{{s}}^2() of the bottom production cross-section in e+ e- annihilation.


pdgid: Q005M
text:
MCNEILE 2004 use lattice QCD with dynamical light quarks and a static heavy quark to compute the masses of heavy-light mesons.


pdgid: Q005M
text:
BAUER 2003 determine the b quark mass by a global fit to B decay observables. The experimental data includes lepton energy and hadron invariant mass moments in semileptonic B --> X_c lepton nu_lepton decay, and the inclusive photon spectrum in B --> X_s gamma decay. The theoretical expressions used are of order 1/m**3, and alpha(s)**2beta(0).


pdgid: Q005M
text:
CORCELLA 2003 determines mbar_{{b}} using sum rules computed to order alpha(s)**2. Includes charm quark mass effects.


pdgid: Q005M
text:
MAHMOOD 2003 determines m(b)**1S by a fit to the lepton energy moments in B --> X_c lepton nu_lepton decay. The theoretical expressions used are of order 1/m**3 and alpha(s)**2beta(0). We have converted their result to the MSbar scheme.


pdgid: Q005M
text:
BRAMBILLA 2002 determine mbar_{{b}}(mbar_{{b}}) from a computation of the Upsilon(1S) mass to order alpha_{{s}}^4(), including finite m_{{c}} corrections.


pdgid: Q005A00
text:
CHAKRABORTY 2015 determine mass(b)/mass(s) from lattice QCD using the HISQ action and including n_{{f}} = 2+1+1 flavors of sea quarks.


pdgid: Q007TP
text:
AAD 2025H based on 140 fb^{-1} of p p data at sqrt(s) = 13 TeV. The error is the sum of the systematic (+-0.46) and statistical (+-0.27) uncertainties. The mean of the invariant mass of the reconstructed large-radius jet is simultaneously fitted with m_{{jj}} and m_{{tj}} to reduce the uncertainties from jet-energy scale and modelling of the recoil in the top decay.


pdgid: Q007TP
text:
HAYRAPETYAN 2024F based on up to 5 and 20 fb^{-1} of p p data at sqrt(s) = 7 and 8 TeV, respectively. The combination includes 15 input measurements in t tbar events that exploit both semileptonic and hadronic decays of the top quark as well as t-channel single-top events.


pdgid: Q007TP
text:
AAD 2023N based on 36.1 fb^{-1} of p p data at sqrt(s) = 13 TeV. The second error is  the sum of systematic (+-0.66) and that from changing parton-shower gluon recoil scheme  (+-0.25) uncertainties. The distribution of the invariant mass mass(lepton mu) (lepton from W and mu from b-hadron decay) is used, which is less sensitive to jet energy uncertainties and top production modelling.


pdgid: Q007TP
text:
TUMASYAN 2023BB based on 36.3 fb^{-1} of p p data at sqrt(s) = 13 TeV. For each event, the mass is reconstructed from a kinematic fit of the decay products to a t tbar hypothesis. A profile likelihood method is applied using up to four observables per event.


pdgid: Q007TP
text:
TUMASYAN 2023Z based on 138 fb^{-1} of p p data at sqrt(s) = 13 TeV. The second error is the sum of experimental (+-0.61), model (+-0.47), and theoretical (+-0.23) uncertainties. The products of the hadronic decay of a top quark with pT > 400 GeV, in the lepton + jets channel of t tbar, are reconstructed as a single jet. The top quark mass is determined from the normalized differential cross section measurement in the mass(jet) distribution.


pdgid: Q007TP
text:
TUMASYAN 2021G based on 35.9 fb^{-1} of p p data at sqrt(s) = 13 TeV. Events are  selected by requiring 1lepton + 2jets(1b jet) final state.


pdgid: Q007TP
text:
SIRUNYAN 2020AR based on 35.9 fb^{-1} of p p data at sqrt(s) = 13 TeV. The products of the hadronic decay of a top quark with pT > 400 GeV, in the lepton + jets channel of t tbar are reconstructed as a single jet. The top quark mass is determined from the normalized differential cross section measurement in the mass(jet) distribution.


pdgid: Q007TP
text:
SIRUNYAN 2019AP based on 35.9 fb^{-1} of p p data at sqrt(s) = 13 TeV. A kinematical fit is applied to each event assuming the signal event topology. mass(t) is determined simultaneously with a jet energy scale factor (JSF). The second error represents stat.+JSF. Modeling uncertainties are larger than in the measurements at sqrt(s) = 7 and 8 TeV because of the use of new alternative color reconnection models.


pdgid: Q007TP
text:
SIRUNYAN 2019AR based on 35.9 fb^{-1} of p p data at sqrt(s) = 13 TeV. Obtained from a simultaneous fit of the cross section and the top quark mass in the POWHEG simulation. The cross section is used also to extract the MSbar mass and the strong coupling constant for different PDF sets.


pdgid: Q007TP
text:
TEVEWWG 2016 is the latest Tevatron average (July 2016) provided by the Tevatron Electroweak Working Group. It takes correlated uncertainties into account and has a chi^2 of 10.8 for 11 degrees of freedom.


pdgid: Q007TP
text:
AABOUD 2019AC based on 20.2 fb**-1 in p p collisions at sqrt(s) = 8 TeV. Uses optimized event selection to suppress less-well-reconstructed events and template fits to determine mass(t) together with a global jet energy scale factor and a relative b-to-light-jet energy scale factor.


pdgid: Q007TP
text:
AABOUD 2019AC is an ATLAS combination of 7 and 8 TeV top-quark mass determination in the dilepton, lepton + jets, and all jets channels.


pdgid: Q007TP
text:
SIRUNYAN 2019AP based on 35.9 fb^{-1} of p p data at sqrt(s) = 13 TeV. A combined measurement using the lepton+jets and all-jets channels through a single likelihood function. See SIRUNYAN 2018DE.


pdgid: Q007TP
text:
SIRUNYAN 2018DE based on 35.9 fb^{-1} of p p data at sqrt(s) = 13 TeV. mass(t) is determined simultaneously with an overall jet energy scale factor constrained by the mass of the hadronically decayed W. Compared to the Run 1 analysis a more advanced treatment of modeling uncertainties are employed, in particular concerning color-reconnection models. Superseded by TUMASYAN 2023BB.


pdgid: Q007TP
text:
AABOUD 2017AH based on 20.2 fb**-1 of p p data at sqrt(s) = 8 TeV. Uses template fits to the ratio of the masses of three-jets (from t candidate) and dijets (from W candidate), to suppress jet energy scale uncertainty. Large QCD background is modelled using a data-driven method.


pdgid: Q007TP
text:
ABAZOV 2017B is a combination of measurements of the top quark mass by D0 in the lepton+jets and dilepton channels, using all data collected in Run I (1992 -- 1996) at sqrt(s) = 1.8 TeV and Run II (2001 -- 2011) at sqrt(s) = 1.96 TeV of the Tevatron, corresponding to integrated luminosities of 0.1 fb^{-1} and 9.7 fb^{-1}, respectively.


pdgid: Q007TP
text:
SIRUNYAN 2017L based on 19.7 fb^{-1} of p p data at sqrt(s) = 8 TeV.  mass(t) is reconstructed from a fit to the invariant mass distribution of mu nu b, where  p_{{T}}^miss and W mass constraint are used to reconstruct nu momentum. The number of  events for various contributions, except for the t-channel single top one, are fixed to the  values extracted from simulation. Superseded by TUMASYAN 2021G.


pdgid: Q007TP
text:
SIRUNYAN 2017N based on 19.7 fb^{-1} of p p data at sqrt(s) = 8 TeV. The fully hadronic decay of a highly-boosted t is reconstructed in the lepton+jets channel and unfolded at the particle level. The sensitivity of the peak position of the m_jet distribution is used to test quality of the modelling by the simulation.


pdgid: Q007TP
text:
SIRUNYAN 2017O based on 19.7 fb^{-1} of p p data at sqrt(s) = 8 TeV. Analysis is based on the kinematical observables M(b lepton), M_T2 and M(b lepton nu). A fit is performed to determine mass(t) and an overall jet energy scale factor simultaneously.


pdgid: Q007TP
text:
AABOUD 2016T based on 20.2 fb**-1 of p p data at sqrt(s) = 8 TeV. The analysis is refined using the p_{{T}} and invariant mass distributions of lepton+b-jet system. A combination with measurements from sqrt(s) = 7 TeV data in the dilepton and lepton+jets channels gives 172.84+-0.34+-0.61 GeV.


pdgid: Q007TP
text:
AABOUD 2016T is an ATLAS combination of 8 TeV top-quark mass in the dilepton channel with previous measurements from sqrt(s) = 7 TeV data in the dilepton and lepton + jets channels.


pdgid: Q007TP
text:
ABAZOV 2016 based on 9.7 fb**-1 of data in p pbar collisions at sqrt(s) = 1.96 TeV. Employs improved fit to  minimize statistical errors and improved jet energy calibration, using lepton + jets mode, which  reduces error of jet energy scale. Based on previous determination in ABAZOV 2012AB with increased integrated luminosity and improved fit and calibrations.


pdgid: Q007TP
text:
ABAZOV 2016D based on 9.7 fb**-1 of data in p pbar collisions at sqrt(s) = 1.96 TeV, using the matrix element technique. Based on previous determination in ABAZOV 2011R with increased integrated luminosity. There is a strong correlation with the determination in ABAZOV 2016. (See ABAZOV 2017B.)


pdgid: Q007TP
text:
KHACHATRYAN 2016AK based on 19.7 fb**-1 of p p data at sqrt(s) = 8 TeV. Combination of the three top mass measurements in KHACHATRYAN 2016AK and with the CMS results at sqrt(s) = 7 TeV gives 172.44+-0.13+-0.47 GeV.


pdgid: Q007TP
text:
KHACHATRYAN 2016AK based on 19.7 fb^{-1} of p p data at sqrt(s) = 8 TeV. Combination of the three top mass measurements in KHACHATRYAN 2016AK and with the CMS results at sqrt(s) = 7 TeV.


pdgid: Q007TP
text:
KHACHATRYAN 2016AL based on 19.7 fb**-1 in p p collisions at sqrt(s) = 8 TeV. Determined from the invariant mass distribution of leptons and reconstructed secondary vertices from b decays using only charged particles. The uncertainty is dominated by modeling of b fragmentation and top p_{{T}} distribution.


pdgid: Q007TP
text:
KHACHATRYAN 2016CB based on 666 candidate reconstructed events corresponding to 19.7 fb**-1 of p p data at sqrt(s) = 8 TeV. The measurement exploits correlation of mass(t) with M(J/psi lepton) in the same top quark decay, using a high-purity event sample. A study on modeling of b-quark fragmentation is given in Sec.3.3.


pdgid: Q007TP
text:
AAD 2015AW based on 4.6 fb**-1 of p p data at sqrt(s) = 7 TeV. Uses template fits to the ratio of the  masses of three-jets (from t candidate) and dijets (from W candidate). Large background from multijet production is modeled with data-driven methods.


pdgid: Q007TP
text:
AAD 2015BF based on 4.6 fb**-1 in p p collisions at sqrt(s) = 7 TeV. Using a three-dimensional template likelihood technique the lepton plus jets (>=1b-tagged) channel gives 172.33+-0.75+-1.02 GeV, while exploiting a one dimensional template method using mass(lepton b) the dilepton channel (1 or 2b-tags) gives 173.79+-0.54+-1.30 GeV.  The results are combined.


pdgid: Q007TP
text:
AALTONEN 2015D based on 9.1 fb**-1 of p pbar data at sqrt(s) = 1.96 TeV. Uses a template technique to fit a distribution of a variable defined by a linear combination of variables sensitive and insensitive to jet energy scale to optimize reduction of systematic errors. b-tagged and non-b-tagged events are separately analyzed and combined.


pdgid: Q007TP
text:
Based on 9.3 fb**-1 of p pbar data at sqrt(s) = 1.96 TeV. Multivariate algorithm is used to discriminate signal from backgrounds, and templates are used to measure mass(t).


