# pdgfootnote

pdgid: S056HEE
text:
BERGER 1985B looked for effect of spin-0 boson exchange in e+ e- --> e+ e- and mu+ mu- at Ecm = 34.7 GeV.  See Fig.5 for excluded region in the mass(X0)-Gamma(X0) plane.


pdgid: S056HEE
text:
ADEVA 1984 and BEHREND 1984C have Ecm = 39.8-45.5 GeV.  MARK-J searched X0 in e+ e- --> hadrons, 2gamma, mu+ mu-, e+ e- and CELLO in the same channels plus tau pair.  No narrow or broad X0 is found in the energy range.  They also searched for the effect of X0 with mass(X) >Ecm. The second limits are from Bhabha data and for spin-0 singlet.  The same limits apply for Gamma(X0 --> e+ e-) = 2 MeV if X0 is a spin-0 doublet.  The second limit of BEHREND 1984C was read off from their figure 2. The original papers also list limits in other channels.


pdgid: S056REE
text:
Limit is for mass(X0) = 56 -- 61.5 GeV and is valid for Gamma(X0)<<100 MeV. See their Fig.5 for limits for Gamma = 1,2 GeV.


pdgid: S056REE
text:
Limit is valid for Gamma(X0)<<100 MeV.  See paper for limits for Gamma = 1 GeV and those for J = 2 resonances.


pdgid: S056REE
text:
STERNER 1993 limit is for mass(X0) = 57 -- 59.6 GeV and is valid for Gamma(X0)<100 MeV. See their Fig.2 for limits for Gamma = 1,3 GeV.


pdgid: S056EPX
text:
CHEKANOV 2002B search for photoproduction of X decaying into dijets in e p collisions.  See their Fig.5 for the limit on the photoproduction cross section.


pdgid: S056REG
text:
ABBIENDI 2003D measure the e+ e- --> gamma gamma gamma cross section at sqrt(s)=181 -- 209 GeV.  The upper bound on the production cross section, sigma(e+ e- --> X0 gamma) times the branching ratio for X0 --> gamma gamma, is less than 0.03pb at 95%CL for X0 masses between 20 and 180 GeV.  See their Fig.9b for the limits in the mass-cross section plane.


pdgid: S056REG
text:
ABREU 2000Z is from the single photon cross section at sqrt(s)=183, 189GeV. The production cross section upper limit is less than 0.3pb for X0 mass between 40 and 160 GeV.  See their Fig.4 for the limit in mass-cross section plane.


pdgid: S056REG
text:
ADAM 1996C is from the single photon production cross at sqrt(s)=130, 136 GeV.  The upper bound is less than 3pb for X0 masses between 60 and 130 GeV.  See their Fig.5 for the exact bound on the cross section CS(e+ e- --> gamma X0).


pdgid: S056ZFR
text:
ADRIANI 1992F give sigma_{{Z}}.B(Z --> q qbar X0) . B(X0 --> gamma gamma)<(0.75 -- 1.5)pb (95%CL) for mass(X0) = 10 -- 70 GeV. The limit is 1pb at 60 GeV.


pdgid: S056PPW
text:
AALTONEN 2013AA search for X0 production associated with W (or Z) in p pbar collisions at Ecm = 1.96 TeV. The upper limit on the cross section CS(p pbar --> W X0) is 2.2 pb for M(X0) = 145 GeV.


pdgid: S056PPW
text:
CHATRCHYAN 2012BR search for X0 production associated with W in p p collisions at Ecm = 7 TeV. The  upper limit on the cross section is 5.0 pb at 95% CL for  mass(X0) = 150 GeV.


pdgid: S056PPW
text:
ABAZOV 2011I search for X0 production associated with W in p pbar collisions at Ecm = 1.96 TeV. The 95% CL upper limit on the cross section ranges from 2.57 to 1.28 pb for X0 mass between 110 and 170 GeV.


pdgid: S056PPW
text:
ABE 1997W search for X0 production associated with W in p pbar collisions at Ecm=1.8 TeV. The 95%CL upper limit on the production cross section times the branching ratio for X0 --> b bbar ranges from 14 to 19pb for X0 mass between 70 and 120 GeV. See their Fig.3 for upper limits of the production cross section as a function of mass(X0).


pdgid: S056ONI
text:
ABLIKIM 2024G search for a muonphilic scalar X_{{0}}() or vector X_{{1}} boson in decays of  J/psi --> mu+ mu- + invisible. See their Fig. 3 for limits in the mass coupling plane.


pdgid: S056ONI
text:
BALEST 1995 three-body limit is for phase-space photon energy distribution and angular distribution same as for Upsilon --> g g gamma.


pdgid: S056HDC
text:
AAD 2024BQ search for X0 production via H --> X0 X0 --> b bbar tau+ tau- in p p  collisions at sqrt(s) = 13 TeV. See their Fig. 10 for limits on .


pdgid: S056HDC
text:
HAYRAPETYAN 2024AA search for X0 production via H(125) --> X0 X0 --> b bbar b bbar in  p p collisions at sqrt(s) = 13 TeV. See their Fig. 3 for limits on .


pdgid: S056HDC
text:
AAD 2022J search for X0 production via H(125) --> X0 X0 / Z X0 --> 4lepton in p p    collisions at sqrt(s) = 13 TeV. X0 --> lepton+ lepton- decay is assumed. See their Fig. 13  and Fig. 17 for limits on  in  H(125) --> X0 X0  and H(125) --> Z X0 channels.


pdgid: S056HDC
text:
AABOUD 2018AP use p p collision data at sqrt(s) = 13 TeV. X0 --> lepton+ lepton-  decay is assumed. See their Fig. 9 for limits on sigma(H(125)).B(Z X0).


pdgid: S056HDC
text:
AABOUD 2018AP use p p collision data at sqrt(s) = 13 TeV. X0 --> lepton+ lepton-  decay is assumed. See their Fig. 10 for limits on sigma(H(125)).B(X0 X0).


pdgid: S029AD2
text:
ABLIKIM 2024AK search for eta^' decays to axions in the mass range 0 to 500 MeV using the  BESIII detector at the Beijing Electron-Positron Collider. See Fig. 9b for mass-dependent limits.


pdgid: S029AD2
text:
ABLIKIM 2024G search for muonphilic vector or scalar X0 particles with masses between 1  and 1000 MeV in J/psi decays at the BESIII detector. See their Fig. 3 for mass-dependent limits  on the scalar/vector couplings under three different models.


pdgid: S029AD2
text:
ABLIKIM 2024M search for eta and eta^' decays to dark photons in the mass range 0 to  0.7 GeV using the BESIII detector at the Beijing Electron-Positron Collider. The quoted limit is  for eta^' --> gamma X0. See Fig. 7 a and b for mass-dependent limits.


pdgid: S029AD2
text:
CORTINA-GIL 2024 use K+ --> pi+ gamma gamma events in NA62 to constrain 210 to 350  MeV-mass axions coupled to gluons, which promptly decay to gamma gamma.  See their Fig. 8 for mass-dependent limits.


pdgid: S029AD2
text:
SADOVSKY 2024 report results from the OKA collaboration on a missing-mass search for  invisible axions in K+ decays to pions. The quoted limit applies at mass(A0) ~= 200 MeV.  See their Fig. 6 for mass-dependent limits up to 200 MeV.


pdgid: S029AD2
text:
ADACHI 2023K quoted limit is for mass(X0) ~= 3 GeV, ctau(X0)  = 1 cm, and the decay channel X0 --> e+ e-. See their Fig. 2 for limits with different  lifetimes and decay channels, X0 -->  mu+ mu- , pi+ pi- , K+ K-.


pdgid: S029AD2
text:
ADACHI 2023K quoted limit is for mass(X0) ~= 2 GeV, ctau(X0)  = 1 cm, and the decay channel X0 --> e+ e-. See their Fig. 2 for limits with different  lifetimes and decay channels, X0 --> mu+ mu- , pi+ pi- , K+ K-.


pdgid: S029AD2
text:
LEES 2022B quoted limit is for mass(A0) =  3.9 GeV, assuming the promptly decaying axion.   Limits of O(E-7) are obtained for mass(A0) = 0.175 -- 4.78 GeV. See their  Figs.3 and 4   for mass and lifetime dependent limits.


pdgid: S029AD2
text:
ABRATENKO 2021 quoted limit is for mass(X0) = 150 MeV and the lifetime   ctau(X0) = 80 m. See their Fig. 4 for the limits in the range of  mass(X0) =  10 -- 210 MeV.


pdgid: S029AD2
text:
CORTINA-GIL 2021 quoted limit is for mass(X0) = 370 MeV. Limits from O(E-5) and  O(E-6) are obtained for mass(X0) = 10 -- 370 MeV (see their Fig. 7).


pdgid: S029AD2
text:
CORTINA-GIL 2021A quoted limit is for mass(X0) = 160 -- 250 MeV. Limits between  5E-11 and 2E-10 are obtained in the range of mass(X0) = 0 -- 110 and 154 -- 260 MeV,  assuming stable or invisibly decaying X0. See their Fig. 4 for mass- and lifetime-dependent  limits.


pdgid: S029AD2
text:
CORTINA-GIL 2021C quoted limit is for mass(X0) = 130 -- 140 MeV, and limits of   9E-10 -- 6E-7 are obtained in the mass range of mass(X0) = 110 -- 155 MeV,  assuming  X0 escapes detection. See their Fig. 6 for mass- and lifetime-dependent limits.


pdgid: S029AD2
text:
PARK 2021 look for dark photons produced by decays of B0 through off-shell Higgs-dark  Higgs mixing. See their Fig. 5 for limits in the range of mass(X0) = 0.01 -- 2.62 GeV.


pdgid: S029AD2
text:
AHN 2019 is an update of AHN 2017 from a new data set. See their Fig. 4 for the limits  in the range of mass(X0) = 0 -- 250 MeV.


pdgid: S029AD2
text:
AAIJ 2017AQ limit is for meanlife(X0) = 10 ps. See their Fig. 4 for limits in the range of  mass(X0) = 250 -- 4700 MeV and meanlife(X0) = 0.1 -- 1000 ps.


pdgid: S029AD2
text:
BATLEY 2017 limit is for mass(X0) = 216 MeV and meanlife(X0) <= 10 ps. See their Fig.  4(c) for limits in the range of mass(X0) = 211 -- 354 MeV and longer lifetimes.


pdgid: S029AD2
text:
WON 2016 look for a vector boson coupled to baryon number. Derived limits on alpha^'  < E-3 -- E-2 for mass(X0) = 290 -- 520 MeV at 95% CL. See their Fig. 4  for mass-dependent limits.


pdgid: S029AD2
text:
AAIJ 2015AZ limit is for meanlife(X0) = 10 ps and mass(X0) = 214 -- 4350 MeV. See  their Fig. 4 for mass- and lifetime-dependent limits.


pdgid: S029AD2
text:
ADLARSON 2013 limits between 2.0E-5 and 1.5E-6 are obtained for mass(X0) = 20 -- 100  MeV (see their Fig. 8). Angular momentum conservation requires that X0 has spin >= 1.


pdgid: S029AD2
text:
BABUSCI 2013B limit is for B(phi --> eta X0).B(X0 --> e+ e-) and applies  to mass(X0) = 410 MeV. It is derived by analyzing eta --> pi0 pi0 pi0 and pi- pi+ pi0.  Limits between 1E-6 and 2E-8 are obtained for mass(X0) <= 450 MeV (see their Fig. 6).


pdgid: S029AD2
text:
ARCHILLI 2012 analyzed eta --> pi+ pi- pi0 decays. Derived limits on alpha^'/alpha < 2E-5  for mass(X0) = 50 -- 420 MeV at 90% CL. See their Fig. 8 for mass-dependent limits.


pdgid: S029AD2
text:
GNINENKO 2012A limit is for B(pi0 --> gamma X0).B(X0 --> e+ e-) and  applies for mass(X0) = 90 MeV and meanlife(X0) ~= 1E-8 sec. Limits between E-8 and  2E-15 are obtained for mass(X0) = 3 -- 120 MeV and meanlife(X0) = 1E-11 -- 1  sec. See their Fig. 3 for limits at different masses and lifetimes.


pdgid: S029AD2
text:
GNINENKO 2012B limit is for B(eta --> gamma X0).B(X0 --> e+ e-) and  applies for  mass(X0) = 100 MeV and meanlife(X0) ~= 6E-9 sec. Limits between  E-5 and 3E-14 are  obtained for mass(X0) ~< 550 MeV and meanlife(X0) = E-10 -- 10  sec. See their Fig. 5  for limits at different mass and lifetime and for eta^' decays.


pdgid: S029AD2
text:
ADLER 2004 limit applies for a mass near 180 MeV. For other masses in the range mass(X0) =  150 -- 250 MeV the limit is less restrictive, but still improves ADLER 2002C and  ATIYA 1993B.


pdgid: S029AD2
text:
The quoted limit is for mass(X0) = 0 -- 80 MeV. See their Fig. 5 for the limit at higher mass. The branching fraction limit assumes pure phase space decay distributions.


pdgid: S029AD2
text:
ALTEGOER 1998 looked for X0 from pi0 decay which penetrate the shielding and convert to pi0 in the external Coulomb field of a nucleus.


pdgid: S029AD2
text:
KITCHING 1997 limit is for B(K+ --> pi+ X0).B(X0 --> gamma gamma) and applies for mass(X0)~=50 MeV, tau(X0)<10**-10s. Limits are provided for 0<mass(X0)<100 MeV, tau(X0)<10**-8s.


pdgid: S029AD2
text:
ADLER 1996 looked for a peak in missing-mass distribution. This work is an update of ATIYA 1993.  The limit is for massless stable X0 particles and extends to mass(X0)=80 MeV at the same level.  See paper for dependence on finite lifetime.


pdgid: S029AD2
text:
MEIJERDREES 1994 limit is based on inclusive photon spectrum and is independent of X0  decay modes. It applies to tau(X0)>10**-23sec.


pdgid: S029AD2
text:
ATIYA 1993B looked for a peak in missing mass distribution. The bound applies for stable X0 of mass(X0)=150 -- 250 MeV, and the limit becomes stronger (10**-8) for mass(X0)=180 -- 240 MeV.


pdgid: S029AD2
text:
NG 1993 studied the production of X0 via  gamma gamma --> pi0 --> gamma X0 in the early universe at T~=1 MeV. The bound  on extra neutrinos from nucleosynthesis DeltaN_{{nu}}<0.3 (WALKER 1991) is  employed.  It applies to mass(X0)<<1 MeV in order to be relativistic down to nucleosynthesis  temperature. See paper for heavier X0.


pdgid: S029AD2
text:
ALLIEGRO 1992 limit applies for mass(X0)=150 -- 340 MeV and is the branching ratio times the decay probability. Limit is <1.5E-8 at 99%CL.


pdgid: S029AD2
text:
ATIYA 1992 looked for a peak in missing mass distribution. The limit applies to mass(X0)=0 -- 130 MeV in the narrow resonance limit.  See paper for the dependence on lifetime.  Covariance requires X0 to be a vector particle.


pdgid: S029AD2
text:
BARABASH 1992 is a beam dump experiment that searched for a light Higgs. Limits between  1E-12 and 1E-7 are obtained for 3 < mass(X0) < 40 MeV.


pdgid: S029AD2
text:
MEIJERDREES 1992 limit applies for meanlife(X0) = 10**-23 -- 10**-11sec. Limits between 2E-4 and 4E-6 are obtained for mass(X0) = 25 -- 120 MeV. Angular momentum conservation requires that X0 has spin >=1.


pdgid: S029AD2
text:
ATIYA 1990B limit is for B(K+ --> pi+ X0).B(X0 --> gamma gamma) and applies for mass(X0) = 50 MeV, meanlife(X0) < 10**-10s.  Limits are also provided for 0 < mass(X0) < 100 MeV, meanlife(X0) < 10**-8s.


pdgid: S029AD2
text:
KORENCHENKO 1987 limit assumes mass(A0) = 1.7 MeV, meanlife(A0) ~< 10**-12 s, and B(A0 --> e+ e-) = 1.


pdgid: S029AD2
text:
EICHLER 1986 looked for pi+ --> e+ nu A0 followed by A0 --> e+ e-.  Limits on the branching fraction depend on the mass and and lifetime of A0.  The quoted limits are valid when tau(A0)~>3.E-10s if the decays are kinematically allowed.


pdgid: S029AD2
text:
YAMAZAKI 1984 looked for a discrete line in K+ --> pi+ X.  Sensitive to wide mass range (5-300 MeV), independent of whether X decays promptly or not.


pdgid: S029AD2
text:
ASANO 1982 at KEK set limits for B(K+ --> pi+ X0) for mass(X0) <100 MeV as BR <4.E-8 for tau(X0 --> n gamma's) >1.E-9 s, BR <1.4E-6 for tau <1.E-9s.


pdgid: S029AD2
text:
ZHITNITSKII 1979 argue that a heavy axion predicted by YANG 1978 (3 <m <40 MeV) contradicts experimental muon anomalous magnetic moments.


pdgid: S029AXQ
text:
ABLIKIM 2023E obtained limits in the range of  8.3E-8 -- 1.8E-6 for  0.165  GeV  <=  mass(A0) <=2.84 GeV. See their Fig. 5 for mass-dependent limits.


pdgid: S029AXQ
text:
JIA 2022 limits between 3.1E-7 -- 1.6E-5 were obtained for 0.22 GeV < mass(A0)  < 9.2 GeV. See their Fig. 4 for mass-dependent limits.


pdgid: S029AXQ
text:
ABLIKIM 2016E limits between 2.8 -- 495.3E-8 were obtained  for 0.212 GeV <  mass(A0) < 3.0 GeV. See their Fig. 5 for mass-dependent limits.


pdgid: S029AXQ
text:
ABLIKIM 2012 derived limits between 4E-7 -- 2.1E-5  for 0.212 GeV < mass(A0)  < 3.0 GeV. See their Fig. 2(c) for mass-dependent limits.


pdgid: S029AXQ
text:
The first DRUZHININ 1987 limit is valid when meanlife(A0)/mass(A0) < 3E-13 s/MeV and mass(A0) < 20 MeV.


pdgid: S029AXQ
text:
The second DRUZHININ 1987 limit is valid when meanlife(A0)/mass(A0) < 5E-13 s/MeV and mass(A0) < 20 MeV.


pdgid: S029AXQ
text:
The third DRUZHININ 1987 limit is valid when meanlife(A0)/mass(A0) >7E-12 s/MeV and mass(A0) < 200 MeV.


pdgid: S029AXQ
text:
EDWARDS 1982 looked for J/psi --> gamma A0 decays by looking for events with a single gamma [of energy ~1/2 the J/psi(1S) mass],


pdgid: S029AXD
text:
BADERTSCHER 2002 looked for a three-body decay of ortho-positronium into a photon and two penetrating (neutral or milli-charged) particles.


pdgid: S029AXD
text:
The TSUCHIAKI 1990 limit is based on inclusive photon spectrum and is independent of A0 decay modes.


pdgid: S029AXD
text:
ORITO 1989 limit translates to g(A0 e e)**2/4pi < 6.2E-10.  Somewhat more sensitive limits are obtained for larger mass(A0): B < 7.6E-6 at 100 keV.


pdgid: S029AXD
text:
AMALDI 1985 set limits B(A0 gamma) / B(gamma gamma gamma) < (1-5)*10**-6 for mass(A0) = 900-100 keV which are about 1/10 of the CARBONI 1983 limits.


pdgid: S029AXD
text:
CARBONI 1983 looked for orthopositronium --> A0 gamma.  Set limit for A0 electron coupling squared, g(e e A0)**2/(4*pi) <6.E-10-7.E-9 for mass(A0) from 150-900 keV (CL = 99.7%). This is about 1/10 of the bound from g-2 experiments.


pdgid: S029AXG
text:
ADHIKARI 2022C search for A0 --> gamma gamma and A0 --> pi+ pi- pi0 decays, and set  limits of f(A0) ~< 0.5 -- 14 GeV at 90% CL. See their Fig. 4  for mass-dependent limits.


pdgid: S029AXG
text:
BASSOMPIERRE 1995 is an extension of BASSOMPIERRE 1993. They looked for a peak in the invariant mass of e+ e- pairs in the region mass(e+ e-) = 1.8+-0.2 MeV. They obtained bounds on the production rate A0 for tau(A0) = 10**-18 -- 10**-9sec. They also found an excess of events in the range mass(e+ e-) = 2.1 -- 3.5 MeV.


pdgid: S029AXP
text:
AAD 2024AT search for Higgs decays to axions, constraining the effective coupling to photons  between 100 MeV and 62 GeV axion mass. Limit strength is dependent on the effective axion-Higgs  coupling and is strongest at the highest mass. See their Fig. 8 for full limits.


pdgid: S029AXP
text:
AAD 2024BN search for the production of long-lived axion-like particles produced in  proton-proton collisions at the ATLAS detector. See their Fig. 2 for cross-section limits on  benchmark ALP masses between 40 and 55 GeV, as a function of their proper decay length. Limits are  presented for both ALP production from q qbar in association with the production of a vector  boson, and ALP production from top decays.


pdgid: S029AXP
text:
AAD 2024BZ set limits on photo-phobic axion-like particles with masses between 0.1 and 40 GeV  that are radiated from vector bosons and decay into gluons. See their Figs. 11 and 12 for limits on  the ALP couplings to W, Z and gluons.


pdgid: S029AXP
text:
AAD 2024CD search for the production of axion-like particles in association with a  hadronically decaying W or Z and large missing transverse energy in proton-proton  collisions at the ATLAS detector. See their Fig. 7 for upper limits on the vector boson coupling  for an ALP mass of 1 MeV as a function of f(A0).


pdgid: S029AXP
text:
AAD 2024K search for Higgs decays to a Z and an axion-like particle in the mass range 0.1  to 33 GeV. They constrain the axion coupling to photons. See Fig. 3b for mass-dependent limits,  which also depend on the coupling of the Higgs to Z A0.


pdgid: S029AXP
text:
HAYRAPETYAN 2024AZ present results from CMS's search for axion-like particles produced from  Higgs decays then promptly decaying to a dimuon. See their Fig. 6 for limits on the effective ALP  coupling to the SM-like Higgs.


pdgid: S029AXP
text:
HAYRAPETYAN 2024I report a search by CMS for an exotic Higgs decay to an axion-like particle  and a Z, which decay to two photons and two leptons respectively. See Fig. 7 and 8 for  mass-dependent limits on the cross-section for the process and the effective axion coupling in the  mass range 1 to 30 GeV.


pdgid: S029AXP
text:
TUMASYAN 2024C reports results from the CMS and TOTEM collaborations' search for  photon-photon fusion events in proton collisions and the subsequent diphoton events which may occur  via the production of axions. Constraints on the axion to two-photon coupling are presented at the  E-5 GeV**-1 level for axion masses between 500 and 2000 GeV.


pdgid: S029AXP
text:
ACCIARRI 2023 search for axions in the NuMI neutrino beam target, which are produced through  mixings with mesons due to the coupling with gluons, and exclude f(A0) around tens  of TeV for mass(A0) = 0.2 -- 0.9 GeV. They assume a slightly suppressed axion coupling to  muons. See their Fig. 4 for the limits.


pdgid: S029AXP
text:
BERTUZZO 2023 employs an analysis analogous to ACCIARRI 2023. They search for  leptophilic axions primarily produced via tau --> mu A0 and tau --> e A0, and exclude  f(A0) around 1E6 -- 6E7 GeV for mass(A0) = 0.2 -- 1.7 GeV. See  their Fig. 2 for the limits.


pdgid: S029AXP
text:
AAD 2022J set upper limits for the cross sections of H --> A0 A0 --> 4 mu and . See    their Figs. 14 and 17 for the respective mass-dependent limits.


pdgid: S029AXP
text:
TUMASYAN 2022AH set the limits of O(E-6) with respect to the product of the  branching fractions of H --> A0 A0 and A0 --> e+ e- , mu+ mu-. They also derive limits on  the effective axion couplings contributing to H --> A0 A0 and H --> Z A0. See their Figs. 5  and 7 for the limits.


pdgid: S029AXP
text:
TUMASYAN 2022R is analogous to GAVELA 2020, and set a limit on the products of the    axion couplings to gluons and Z bosons as G(A Z Z) G(A g g)    < 6.64E-7 GeV**-2 at 95% CL for f(A0) = 3 TeV and mass(A0)    < 100 GeV. Here we use c(Gtilde) = G(A g g)   f(A0)/4 and  c(Ztilde) = G(A Z Z)   f(A0)/4 to translate their limits. They also set a limit on the product of the   axion couplings to gluons and Z H.  See their Fig. 9 for the f(A0)-dependent   limits.


pdgid: S029AXP
text:
AAD 2021F look for axion production with an energetic jet and large missing pT, and set  a limit on the axion coupling to gluons, c(Gtilde)/f(A0) <  8E-6 GeV**-1 at 95 % CL for mass(A0) = 1 MeV. Using c(Gtilde) =  alpha(s)/8pi, we interpret the limit as f(A0) > 0.4  TeV for alpha(s) ~= 0.08.


pdgid: S029AXP
text:
AAD 2021K look for axion production with an energetic photon and large missing pT, and  set a limit on the axion coupling to a Z boson and photon, G(A Z gamma)  < 5.1E-4 GeV**-1 at 95 % CL for mass(A0) = 1 MeV and assuming  G(A gamma gamma) = 0.


pdgid: S029AXP
text:
AAD 2021N look for axion production using the measurement of light-by-light scattering based   on Pb+Pb collision data. They set the limit on the axion-photon coupling,   G(A gamma gamma) < 5.3E-5 -- 3.4E-4 GeV**-1 at 95 % CL for   mass(A0) = 6 -- 100 GeV. Here we use Lambda(a) =G(A gamma gamma)**-1  to translate their limits.  See their Fig. 9 for mass-dependent limits.


pdgid: S029AXP
text:
CARRA 2021 is analogous to GAVELA 2020, and they use the differential cross sections  for W W and Z gamma production measured with the ATLAS detector to set limits on the  product of the axion couplings to gauge bosons as G(A W W) G(A g g) <  6.2E-7 GeV**-2 and G(A Z gamma) G(A g g) < 3.7E-7  GeV**-2 at 95 % CL for mass(A0) ~< 100 GeV.


pdgid: S029AXP
text:
AAIJ 2020AL look for a light new boson decaying into a pair of muons using the LHCb data with  an integrated luminosity of 5.1 fb**-1, and set limits on the cross section over a range of  mass(X0) = 0.22 -- 3 and 20 -- 60 GeV. See Figs. 8 and 9 for mass-dependent limits.


pdgid: S029AXP
text:
GAVELA 2020 focus on the axion production as an s-channel off shell mediator, and use the Run  2 CMS public data to set limits on the product of the axion couplings to gluons and photons as well  as Z bosons as G(A gamma gamma) G(A g g) < 2.8E-7  GeV**-2 and G(A Z Z) G(A g g) < 9.8E-7 GeV**-2  for mass(A0) ~< 200 GeV. See their Fig.3 for the limits.


pdgid: S029AXP
text:
SIRUNYAN 2019BQ look for the pair production of a new light boson decaying into a pair of  muons, and set limits on the product of the production cross section times branching fraction to  dimuons squared times acceptance over a range of mass(X0) = 0.25 -- 8.5 GeV. See the right  panel of their Fig. 1 for mass-dependent limits.


pdgid: S029AXP
text:
JAIN 2007 claims evidence for A0 --> e+ e- produced in Pb207 collision  on nuclear emulsion (Ag/Br) for m(A0) = 7+-1 or 19+-1 MeV  and tau(A0) <= 10**-13 s.


pdgid: S029AXP
text:
AHMAD 1997 reports a result of APEX Collaboration which studied positron production in U238+Ta232 and U238+Ta181 collisions, without requiring a coincident electron. No narrow lines were found for 250<E(e+)<750 keV.


pdgid: S029AXP
text:
LEINBERGER 1997 (ORANGE Collaboration) at GSI looked for a narrow sum-energy e+ e--line at ~635keV in U238+Ta181 collision.  Limits on the production probability for a narrow sum-energy e+ e- line are set. See their Table2.


pdgid: S029AXP
text:
GANZ 1996 (EPosII Collaboration) has placed upper bounds on the production cross section of e+ e- pairs from U238+Ta181 and U238+Th232 collisions at GSI. See Table2 for limits both for back-to-back and isotropic configurations of e+ e- pairs. These limits rule out the existence of peaks in the e+ e- sum-energy distribution, reported by an earlier version of this experiment.


pdgid: S029AXP
text:
KAMEL 1996 looked for e+ e- pairs from the collision of S32 (200GeV/nucleon) and emulsion.  No evidence of mass peaks is found in the region of sensitivity mass(e e)>2 MeV.


pdgid: S029AXP
text:
BLUEMLEIN 1992 is a proton beam dump experiment at Serpukhov with a secondary target to induce Bethe-Heitler production of e+ e- or mu+ mu- from the produce A0.  See Fig.5 for the excluded region in mass(A0)-x plane. For the standard axion, 0.3<x<25 is excluded at 95% CL.  If combined with BLUEMLEIN 1991, 0.008<x<32 is excluded.


pdgid: S029AXP
text:
MEIJERDREES 1992 give Gamma(pi- p --> n A0).B(A0 --> e+ e-)/Gamma(pi- p --> all) <10**-5 (90% CL) for mass(A0) = 100 MeV, meanlife(A0) = 10**-11 -- 10**-23sec. Limits ranging from 2.5E-3 to 10**-7 are given for mass(A0) = 25 -- 136 MeV.


pdgid: S029AXP
text:
BLUEMLEIN 1991 is a proton beam dump experiment at Serpukhov.  No candidate event for A0 --> e+ e-, 2gamma are found.  Fig.6 gives the excluded region in mass(A0)-x plane (x= tan(beta) = v(2)/v(1)). Standard axion is excluded for 0.2 < mass(A0) < 3.2 MeV for most x>1, 0.2 -- 11 MeV for most x<1.


pdgid: S029AXP
text:
FAISSNER 1989 searched for A0 --> e+ e- in a proton beam dump experiment at SIN.  No excess of events was observed over the background.  A standard axion with mass 2mass(e)-20 MeV is excluded. Lower limit on f(A0) of ~10**4 GeV is given for mass(A0) = 2mass(e)-20 MeV.


pdgid: S029AXP
text:
DEBOER 1988 reanalyze EL-NADI 1988 data and claim evidence for three distinct states with mass ~1.1, ~2.1, and ~9 MeV, lifetimes 10**-16-10**-15s decaying to e+ e- and note the similarity of the data with those of a cosmic-ray experiment by Bristol group (B.M.Anand, Proc. of the Royal Society of London, Section A  A22 183 (1953)). For a criticism see PERKINS 1989, who suggests that the events are compatible with pi0 Dalitz decay.  DEBOER 1989B is a reply which contests the criticism.


pdgid: S029AXP
text:
EL-NADI 1988 claim the existence of a neutral particle decaying into e+ e- with mass 1.60+-0.59 MeV, lifetime 0.15+-0.01E-14s, which is produced in heavy ion interactions with emulsion nuclei at ~4 GeV/c/nucleon.


pdgid: S029AXP
text:
FAISSNER 1988 is a proton beam dump experiment at SIN.  They found no candidate event for A0 --> gamma gamma.  A standard axion decaying to 2gamma is excluded except for a region x~1.  Lower limit on f(A0) of 10**2-10**3 GeV is given for mass(A0) = 0.1-1 MeV.


pdgid: S029AXP
text:
BADIER 1986 did not find long-lived A0 in 300 GeV pi- Beam Dump Experiment that decays into e+ e- in the mass range mass(A0) = (20-200) MeV, which excludes the A0 decay constant f(A0) in the interval (60-600) GeV. See their figure 6 for excluded region on f(A0)-mass(A0) plane.


pdgid: S029AXP
text:
BERGSMA 1985 look for A0 --> 2gamma, e+ e-, mu+ mu-.  First limit above is for mass(A0) = 1 MeV; second is for 200 MeV.  See their figure 4 for excluded region on f(A0)-mass(A0) plane, where f(A0) is A0 decay constant. For Peccei-Quinn PECCEI 1977 A0, mass(A0) <180 keV and tau >0.037 s.  (CL = 90%). For the axion of FAISSNER 1981B at 250 keV, BERGSMA 1985 expect 15 events but observe zero.


pdgid: S029AXP
text:
FAISSNER 1983 observed 19 1-gamma and 12 2-gamma events where a background of 4.8 and 2.3 respectively is expected.  A small-angle peak is observed even if iron wall is set in front of the decay region.


pdgid: S029AXP
text:
FAISSNER 1983B extrapolate SIN gamma signal to LAMPF nu experimental condition. Resulting 370 gamma's are not at variance with LAMPF upper limit of 450 gamma's.  Derived from LAMPF limit that [dCS(A0)/domega at 90degrees]*mass(A0)/meanlife(A0) <14E-35 cm**2* sr**-1* MeV *ms**-1.


pdgid: S029AXP
text:
FRANK 1983B stress the importance of LAMPF data bins with negative net signal.  By statistical analysis say that LAMPF and SIN-A0 are at variance when extrapolation by phase-space model is done. They find LAMPF upper limit is 248 not 450 gamma's.  See comment on FAISSNER 1983B.


pdgid: S029AXP
text:
HOFFMAN 1983 set CL = 90% limit d(sigma)/dt* B(e+ e-) <3.5E-32 cm**2/GeV**2 for 140 <mass(A0) <160 MeV.  Limit assumes tau(A0) <10**-9 s.


pdgid: S029AXP
text:
FETSCHER 1982 reanalyzes SIN beam-dump data of FAISSNER 1981.  Claims no evidence for axion since 2-gamma peak rate remarkably decreases if iron wall is set in front of the decay region.


pdgid: S029AXP
text:
FAISSNER 1981B is SIN 590 MeV proton beam dump.  Observed 14.5+-5.0 events of 2gamma decay of long-lived neutral penetrating particle with mass(2gamma) ~<1 MeV.  Axion interpretation with eta-A0 mixing gives mass(A0) = 250+-25 keV, tau((2gamma)) = 7.3+-3.7E-3s from above rate. See critical remarks below in comments of FETSCHER 1982, FAISSNER 1983, FAISSNER 1983B, FRANK 1983B, and BERGSMA 1985.  Also see in the next subsection ALEKSEEV 1982B, CAVAIGNAC 1983, and ANANEV 1985.


pdgid: S029AXP
text:
KIM 1981 analyzed 8 candidates for A0 --> 2gamma obtained by Aachen-Padova experiment at CERN with 26 GeV protons on Be.  Estimated axion mass is about 300 keV and lifetime is (0.86~5.6)*10**-3s depending on models.


pdgid: S029AXP
text:
FAISSNER 1980 is SIN beam dump experiment with 590 MeV protons looking for A0 --> e+ e- decay.  Assuming A0/pi0 = 5.5E-7, obtained decay rate limit 20/(A0 mass) MeV/s (CL = 90%), which is about 10**-7 below theory and interpreted as upper limit to mass(A0) <2*mass(e-).


pdgid: S029AXP
text:
JACQUES 1980 is a BNL beam dump experiment.  First limit above comes from nonobservation of excess neutral-current-type events [CS(production)*CS(interaction) <7.E-68 cm**4, CL = 90%].  Second limit is from nonobservation of axion decays into 2gamma's or e+ e-, and for axion mass a few MeV.


pdgid: S029AXP
text:
BECHIS 1979 looked for the axion production in low energy electron Bremsstrahlung and the subsequent decay into either 2gamma or e+ e-.  No signal found.  CL = 90% limits for model parameter(s) are given.


pdgid: S029AXP
text:
DISHAW 1979 is a calorimetric experiment and looks for low energy tail of energy distributions due to energy lost to weakly interacting particles.


pdgid: S029AXP
text:
BELLOTTI 1978 first value comes from search for A0 --> e+ e-.  Second value comes from search for A0 --> 2gamma, assuming mass <2*mass(e-). For any mass satisfying this, limit is above value*(mass**-4). Third value uses data of PL 60B 401 and quotes CS(production)*CS(interaction) < 10**-67 cm**4.


pdgid: S029AXP
text:
DONNELLY 1978 examines data from reactor neutrino experiments of REINES 1976 and GURR 1974 as well as SLAC beam dump experiment.  Evidence is negative.


pdgid: S029AXP
text:
MICELMACHER 1978 finds no evidence of axion existence in reactor experiments of REINES 1976 and GURR 1974.  (See reference under DONNELLY 1978 below).


pdgid: S029AXP
text:
VYSOTSKII 1978 derived lower limit for the axion mass 25 keV from luminosity of the sun and 200 keV from red supergiants.


pdgid: S029AXR
text:
CHANG 2007 looked for monochromatic photons from Primakoff or Compton conversion of axions from  the Kuo-Sheng reactor due to axion coupling to photon or electron, respectively. The search places  model-independent limits on the products G(A gamma gamma)G(A N N) and G(A e e)G(A N N) for m(A0) less than the MeV range.


pdgid: S029AXR
text:
ALTMANN 1995 looked for A0 decaying into e+ e- from the Bugey5 nuclear reactor.  They obtain an upper limit on the A0 production rate of omega(A0)/omega(gamma) *B(A0 --> e+ e-)<10**-16 for mass(A0) = 1.5 MeV at 90% CL.  The limit is weaker for heavier A0.  In the case of a standard axion, this limit excludes a mass in the range 2mass(e)<mass(A0)<4.8 MeV at 90% CL.  See Fig.5 of their paper for exclusion limits of axion-like resonances Z0 in the (mass(X0),f(X0)) plane.


pdgid: S029AXR
text:
KETOV 1986 searched for A0 at the Rovno nuclear power plant.  They found an upper limit on the A0 production probability of 0.8 [100 keV/mass(A0)]**6 *10**-6 per fission.  In the standard axion model, this corresponds to mass(A0) >150 keV.  Not valid for mass(A0) ~> 1 MeV.


pdgid: S029AXR
text:
KOCH 1986 searched for A0 --> gamma gamma at nuclear power reactor Biblis A.  They found an upper limit on the A0 production rate of omega(A0)/omega(gamma(M1)) < 1.5E-10 (CL=95%).  Standard axion with mass(A0) = 250 keV gives 10**-5 for the ratio.  Not valid for mass(A0) >1022 keV.


pdgid: S029AXR
text:
DATAR 1982 looked for A0 --> 2gamma in neutron capture (n p --> d A0) at Tarapur 500 MW reactor.  Sensitive to sum of I =  0 and I =  1 amplitudes. With ZEHNDER 1981 [(I = 0) - (I = 1)] result, assert nonexistence of standard A0.


pdgid: S029ANT
text:
DERBIN 2023 use a thallium garnet bolometric detector to search for the 8.4 keV solar axion  line emitted from the M1 nuclear transition of Tm169. Their limits are equivalent to an  upper bound on the KSVZ and DFSZ axion masses of 141 eV and 244 eV, respectively.


pdgid: S029ANT
text:
DERBIN 2002 looked for the axion emission in an M1 transition in **125mTe  decay.  They looked for a possible presence of a shifted energy spectrum in gamma rays due to the  undetected axion.


pdgid: S029ANT
text:
DEBOER 1997C reanalyzed the existent data on Nuclear M1 transitions and find that a 9MeV boson decaying into e+ e- would explain the excess of events with large opening angles. See also DEBOER 2001 for follow-up experiments.


pdgid: S029ANT
text:
TSUNODA 1995 looked for axion emission when Cf252 undergoes a spontaneous fission, with the axion decaying into e+ e-.  The bound is for mass(A0)=40 MeV.  It improves to 2.5E-5 for mass(A0)=200 MeV.


pdgid: S029ANT
text:
MINOWA 1993 studied chain process,  ^139Ce -->  ^139La* by electron capture and M1 transition of La139* to the ground state.  It does not assume decay modes of A0. The bound applies for mass(A0)<166 keV.


pdgid: S029ANT
text:
The ASANUMA 1990 limit is for the branching fraction of X0 emission per  ^241Am alpha decay and valid for meanlife(X0) < 3E-11s.


pdgid: S029ANT
text:
The DEBOER 1990 limit is for the branching ratio Be8* (18.15 MeV, 1**+) -->  ^8Be A0, A0 --> e+ e- for the mass range mass(A0) = 4-15 MeV.


pdgid: S029ANT
text:
The BINI 1989 limit is for the branching fraction of  ^16O* (6.05 MeV, 0^+) -->  ^16O X0, X0 --> e+ e- for mass(X) = 1.5-3.1 MeV.  meanlife(X0) ~< 10**-11s is assumed.  The spin-parity of X is restricted to 0**+ or 1**-.


pdgid: S029ANT
text:
AVIGNONE 1988 looked for the 1115 keV transition  ^C* -->  ^Cu A0, either from A0 --> 2gamma in-flight decay or from the secondary A0 interactions by Compton and by Primakoff processes.  Limits for axion parameters are obtained for mass(A0) < 1.1 MeV.


pdgid: S029ANT
text:
DATAR 1988 rule out light pseudoscalar particle emission through its decay A0 --> e+ e- in the mass range 1.02-2.5 MeV and lifetime range 10**-13-10**-8s. The above limit is for tau = 5E-13s and m = 1.7 MeV;  see the paper for the tau-m dependence of the limit.


pdgid: S029ANT
text:
The limit is for the branching fraction of  ^16O* (6.05 MeV, 0^+) -->  ^16O X0, X0 --> e+ e- against internal pair conversion for mass(X0) = 1.7 MeV and meanlife(X0) < 10**-11s. Similar limits are obtained for mass(X0) = 1.3-3.2 MeV.  The spin parity of X0 must be either 0**+ or 1**-.  The limit at 1.7 MeV is translated into a limit for the X0-nucleon coupling constant: g(X0 NN)**2/4pi < 2.3E-9.


pdgid: S029ANT
text:
The DOEHNER 1988 limit is for mass(A0) = 1.7 MeV, tau(A0) < 10**-10s.  Limits less than 10**-4 are obtained for mass(A0) = 1.2-2.2 MeV.


pdgid: S029ANT
text:
SAVAGE 1988 looked for A0 that decays into e+ e- in the decay of the 9.17 MeV J**P = 2**+** state in N14, 17.64 MeV state J**P = 1**+** in Be8, and the 18.15 MeV state J**P = 1**+** in Be8. This experiment constrains the isovector coupling of A0 to hadrons, if mass(A0) = (1.1 --> 2.2) MeV and the isoscalar coupling of A0 to hadrons, if mass(A0) = (1.1 --> 2.6) MeV. Both limits are valid only if tau(A0) ~< 1E-11 s.


pdgid: S029ANT
text:
Limits are for Gamma(A0(1.8 MeV))/Gamma(piM1); i.e., for 1.8 MeV axion emission normalized to the rate for internal emission of e+ e- pairs. Valid for meanlife(A0) < 2E-11s. Li6 isovector decay data strongly disfavor PECCEI 1986 model I, whereas the B10 and N14 isoscalar decay data strongly reject PECCEI 1986 model II and III.


pdgid: S029ANT
text:
SAVAGE 1986B looked for A0 that decays into e+ e- in the decay of the 9.17 MeV J**P = 2+ state in N14.  Limit on the branching fraction is valid if meanlife(A0)~<1.E-11s for mass(A0) = (1.1-1.7) MeV.  This experiment constrains the iso-vector coupling of A0 to hadrons.


pdgid: S029ANT
text:
ANANEV 1985 with IBR-2 pulsed reactor exclude standard A0 at CL = 95% masses below 470 keV (Li* decay) and below 2*mass(e) for deuteron* decay.


pdgid: S029ANT
text:
CAVAIGNAC 1983 at Bugey reactor exclude axion at any mass(Nb97*decay) and axion with mass(A0) between 275 and 288 keV (deuteron* decay).


pdgid: S029ANT
text:
ALEKSEEV 1982 with IBR-2 pulsed reactor exclude standard A0 at CL = 95% mass-ranges mass(A0) <400 keV (Li* decay) and 330 keV <mass(A0) <2.2 MeV. (deuteron* decay).


pdgid: S029ANT
text:
LEHMANN 1982 obtained A0 --> 2gamma rate <6.2E-5/s (CL = 95%) excluding mass(A0) between 100 and 1000 keV.


pdgid: S029ANT
text:
ZEHNDER 1982 used Gosgen 2.8GW light-water reactor to check A0 production. No 2gamma peak in Li*, Nb* decay (both single p transition) nor in n capture (combined with previous Ba* negative result) rules out standard A0. Set limit mass(A0) <60 keV for any A0.


pdgid: S029ANT
text:
ZEHNDER 1981 looked for  ^Ba* --> A0  ^Ba transition with A0 --> 2gamma. Obtained 2gamma coincidence rate <2.2E-5/s (CL = 95%) excluding mass(A0) >160 keV (or 200 keV depending on Higgs mixing).


pdgid: S029ANT
text:
CALAPRICE 1979 saw no axion emission from excited states of carbon. Sensitive to axion mass between 1 and 15 MeV.


pdgid: S029AXE
text:
ANDREEV 2021 look for invisible decays of axions coupled to electrons, and set limits on   g(A e e) < 4.6E-6 -- 3.1E-3 for mass(A0) = E-3 -- 1 GeV.  This  limits the axion contribution to the electron g-2  to an order of magnitude  less  than the current experimental uncertainty. See their Figs. 3 and 4 for mass-dependent limits.


pdgid: S029AXE
text:
ANDREEV 2021B set limits on g(A e e) in the range of 6.3E-6 -- 1.6E-3   for mass(A0) = 2 -- 17 MeV at 90% CL. This excludes 6.6E-5 <  g(A e e)  < 1E-4 at mass(A0) = 16.7 MeV corresponding to the ATOMKI  anomaly. See their Fig. 2 for  mass-dependent limits.


pdgid: S029AXE
text:
The listed BROSS 1991 limit is for mass(A0) = 1.14MeV. B(A0 --> e+ e-) =1 assumed.  Excluded domain in the meanlife(A0)-mass(A0) plane extends up to mass(A0) ~~7 MeV (see Fig.5).  Combining with electron g-2 constraint, axions coupling only to e+ e- ruled out for mass(A0) <4.8 MeV (90% CL).


pdgid: S029AXE
text:
GUO 1990 use the same apparatus as BROWN 1986 and improve the previous limit in the shorter lifetime region. Combined with g-2 constraint, axions coupling only to e+ e- are ruled out for mass(A0) < 2.7 MeV (90% CL).


pdgid: S029AXE
text:
BJORKEN 1988 reports limits on axion parameters (f_{{A}}, m_{{A}}, tau_{{A}}) for mass(A0) < 200 MeV from electron beam-dump experiment with production via Primakoff photoproduction, bremsstrahlung from electrons, and resonant annihilation of positrons on atomic electrons.


pdgid: S029AXE
text:
BLINOV 1988 assume zero spin, m = 1.8 MeV and lifetime < 5E-12s and find Gamma(A0 --> gamma gamma)B(A0 --> e+ e-) < 2 eV (CL=90%).


pdgid: S029AXE
text:
Assumes A0 gamma gamma coupling is small and hence Primakoff production is small.  Their figure 2 shows limits on axions for mass(A0) < 15 MeV.


pdgid: S029AXE
text:
Uses electrons in hadronic showers from an incident 800 GeV proton beam.  Limits for mass(A0) < 15 MeV are shown in their figure 3.


pdgid: S029AXE
text:
mass(A0) = 1.8 MeV assumed.  The excluded domain in the meanlife(A0)-mass(A0) plane extends up to mass(A0) ~~ 14 MeV, see their figure 4.


pdgid: S029AXE
text:
The limits are obtained from their figure 3. Also given is the limit on the A0 gamma gamma-A0 e+ e- coupling plane by assuming Primakoff production.


pdgid: S029AEE
text:
HALLIN 1992 quote limits on lifetime, 8E-14--5E-13 sec depending on mass, assuming B(A0 --> e+ e-) = 100%.  They say that TSERTOS 1991 overstated their sensitivity by a factor of 3.


pdgid: S029AEE
text:
HENDERSON 1992C exclude axion with lifetime meanlife(A0)=1.4E-12--4.0E-10s, assuming B(A0 --> e+ e-)=100%. HENDERSON 1992C also exclude a vector boson with =1.4E-12--6.0E-10s.


pdgid: S029AEE
text:
WU 1992 quote limits on lifetime >3.3E-13s assuming B(A0 --> e+ e-)=100%.  They say that TSERTOS 1989 overestimate the limit by a factor of pi/2.  WU 1992 also quote a bound for vector boson, >8.2E-13s.


pdgid: S029AEE
text:
WIDMANN 1991 bound applies exclusively to the case B(A0 --> e+ e-)=1, since the detection efficiency varies substantially as Gamma(A0)(total) changes.  See their Fig.6.


pdgid: S029AEE
text:
JUDGE 1990 excludes an elastic pseudoscalar e+ e- resonance for 4.5E-13s < tau(A0) < 7.5E-12s (95% CL) at mass(A0) = 1.832 MeV. Comparable limits can be set for mass(A0) = 1.776-1.856 MeV.


pdgid: S029AEE
text:
The upper limit listed in TSERTOS 1988 is too large by a factor of 4.  See TSERTOS 1988B, footnote 3.


pdgid: S029AEE
text:
VANKLINKEN 1988 looked for relatively long-lived resonance (tau = 10**-10-10**-12s). The sensitivity is not sufficient to exclude such a narrow resonance.


pdgid: S029AEE
text:
MAIER 1987 obtained limits RGamma ~< 60 eV (100 eV) at mass(A0) ~ 1.64 MeV (1.83 MeV) for energy resolution DeltaEcm ~ 3 keV, where R is the resonance cross section normalized to that of Bhabha scattering, and Gamma = Gamma(e e)**2/Gamma(total). For a discussion implying that DeltaEcm ~ 10keV, see TSERTOS 1989.


pdgid: S029AEE
text:
VONWIMMERSPERG 1987 measured Bhabha scattering for Ecm = 1.37-1.86 MeV and found a possible peak at 1.73 with integral (sigmadEcm) = 14.5+-6.8 keV.b.  For a comment and a reply, see VANKLINKEN 1988B and VONWIMMERSPERG 1988. Also see CONNELL 1988.


pdgid: S029AEG
text:
TRZASKA 1991 also give limits in the range (6.6 -- 30)*10**-3eV (95%CL) for mass(A0) = 1.6 -- 2.0MeV.


pdgid: S029AEG
text:
FOX 1989 measured positron annihilation with an electron in the source material into two photons and found no signal at 1.062 MeV (< 9E-5 of two-photon annihilation at rest).


pdgid: S029XEG
text:
VO 1994 looked for X0 --> gamma gamma gamma decaying at rest.  The precise limits depend on mass(X0). See Fig.2(b) in paper.


pdgid: S029XEG
text:
SKALSEY 1992 also give limits 4.3 for mass(X0) = 1.54 and 7.5 for 1.64 MeV.  The spin of X0 is assumed to be one.


pdgid: S029XGE
text:
MITSUI 1996 looked for a monochromatic gamma. The bound applies for a vector X0 with C=-1 and mass(X0)<200 keV.  They derive an upper bound on e e X0 coupling and hence on the branching ratio B(o-Ps --> gamma gamma X0)<6.2E-6. The bounds weaken for heavier X0.


pdgid: S029XGE
text:
SKALSEY 1995 looked for a monochromatic gamma without an accompanying gamma in e+ e- annihilation.  The bound applies for scalar and vector X0 with C = -1 and mass(X0) =  keV.


pdgid: S029XGE
text:
SKALSEY 1995 reinterpreted the bound on gamma A0 decay of o-Ps by ASAI 1991 where 3% of delayed annihilations are not from 3S1 states.  The bound applies for scalar and vector X0 with C = -1 and mass(X0) = 0 -- 800 keV.


pdgid: S029XGE
text:
ADACHI 1994 looked for a peak in the gamma gamma invariant mass distribution in gamma gamma gamma gamma production from e+ e- annihilation.  The bound applies for mass(X0) = 70 -- 800 keV.


pdgid: S029XGE
text:
ADACHI 1994 looked for a peak in the missing-mass mass distribution in gamma gamma channel, using gamma gamma gamma gamma production from e+ e- annihilation.  The bound applies for mass(X0) <800 keV.


pdgid: S029XGE
text:
ADACHI 1994 looked for a peak in the missing mass distribution in gamma gamma gamma channel, using gamma gamma gamma gamma production from e+ e- annihilation.  The bound applies for mass(X0) = 200 -- 900 keV.


pdgid: S029GB
text:
ADACHI 2023A set limits in the range of 1.1E-3 -- 9.7E-3 for  0 < mass(X0)    < 1.6 GeV on B(tau- --> e- X0)/B(tau- --> e- nubar_e nu_tau).  See their Fig. 2   for mass-dependent limits.


pdgid: S029GB
text:
ADACHI 2023A set limits in the range of 7E-4 -- 1.22E-2 for  0 < mass(X0)     < 1.6 GeV on B(tau- --> mu- X0)/B(tau- --> mu- nubar_mu nu_tau).  See their Fig.   2  for mass-dependent limits.


pdgid: S029GB
text:
FIORILLO 2023 used data from Kamiokande-II and IMB on the neutrino flux from SN1987A to   constrain the universal neutrino Majoron Yukawa coupling, g. They set an upper limit of   g mass(X0) ~< E-9 MeV for Majoron masses 100 eV ~< mass(X0) ~< 100   MeV, using neutrino coalescence as production of Majorons which then decay back to neutrinos. See   their Fig. 1 for the mass-dependent limits.


pdgid: S029GB
text:
SANDNER 2023 study Majoron production via neutrino inverse decay and use Planck data to    constrain the neutrino   Majoron Yukawa coupling to g ~< 2E-13 -- 1E-12 for    Majoron masses mass(X0)  =  1 -- 10 eV.  See their Fig. 1 for mass-dependent limits.


pdgid: S029GB
text:
COLOMA 2022A used the spectral data of Borexino Phase II to constrain the neutrino    non-standard interaction with electrons mediated by a scalar or a pseudoscalar. Limits on the   universal  coupling to neutrinos and electrons between 2E-6 and E-4 are obtained for   mass(X0)  ~< 30 -- 40 MeV.  See their Fig. 6 for mass-dependent limits.


pdgid: S029GB
text:
AGUILAR-AREVALO 2021A quoted limit applies to mass(X0) = 33.9 MeV. Limits between 4.3E-6 and  7.5E-5 are obtained for 0 < mass(X0) < 33.9 MeV. The lifetime of X0 is  assumed to be long enough. See their Fig. 6 for mass-dependent limits.


pdgid: S029GB
text:
AGUILAR-AREVALO 2021A quoted limit applies to mass(X0) = 85 MeV. Limits between 5.2E-8  and 1.4E-6 are  obtained for 0 < mass(X0) < 120 MeV, which improve the limits of  PICCIOTTO 1988  by an order of magnitude. The lifetime of X0 is assumed to be long  enough. See their Fig. 4 for  mass-dependent limits.


pdgid: S029GB
text:
AGUILAR-AREVALO 2020 obtained limits of order E-5 for mass(X0) = 47.8 -- 95.1  MeV. The quoted limit applies to  mass(X0) = 75 MeV. See their Fig. 1 for mass-dependent limits.


pdgid: S029GB
text:
BALDINI 2020 obtained limits for mass(X0) = 20 -- 45 MeV and tau(X0)  < 40 ps, and supersedes BOLTON 1988 for mass(X0) = 20 -- 40 MeV. See their Fig.  17 for mass-dependent limits.


pdgid: S029GB
text:
BAYES 2015 limits are the average over mass(X0) = 13 -- 80 MeV for the isotropic  decay distribution of positrons. See their Fig. 4 and Table II for the mass-dependent limits as  well as the dependence on the decay anisotropy. In particular, they find a limit < 58E-6  at 90% CL for massless familons and for the same asymmetry as normal muon decay, a case not  covered by JODIDIO 1986.


pdgid: S029GB
text:
LATTANZI 2013 use WMAP 9 year data as well as X-ray and gamma-ray observations to derive limits on decaying majoron dark matter. A limit on the decay width Gamma(X0 --> nu nubar) < 6.4E-19 s**-1 at 95% CL is found if majorons make up all of the dark matter.


pdgid: S029GB
text:
LESSA 2007 consider decays of the form Meson lepton nu Majoron and lepton --> lepton^'() nu nubar Majoron and use existing data to derive limits on the neutrino-Majoron Yukawa  couplings g(alpha beta) (alpha,beta = e, mu,tau). Their best limits are |g(e alpha) |**2< 5.5E-6, |g(mu alpha) |**2< 4.5E-5, |g(tau alpha) |**2< 5.5E-2 at CL = 90%.


pdgid: S029GB
text:
FARZAN 2003 set limits on the neutrino Majoron Yukawa coupling, |g(e e)|  < 4E-7, by considering the SN cooling due to the massless Majoron emission via neutrino  coalescence. They also exclude values around E-5 for both g(e mu) and  g(mu mu) using the process nu nu --> X0 X0. See also their Figs. 3 and 4 for  mass-dependent limits.


pdgid: S029GB
text:
DIAZ 1998 studied models of spontaneously broken lepton number with both singlet and triplet Higgses.  They obtain limits on the parameter space from invisible decay Z --> H0 A0 --> X0 X0 X0 X0 X0 and e+ e- --> Z H0 with H0 --> X0 X0.


pdgid: S029GB
text:
BOBRAKOV 1991 searched for anomalous magnetic interactions between polarized electrons expected from the exchange of a massless pseudoscalar boson (arion). A limit x(e)**2 < 2E-4 (95%CL) is found for the effective anomalous magneton parametrized as x(e)(G(F)/8pisqrt(2))**1/2.


pdgid: S029GB
text:
ALBRECHT 1990E limits are for B(tau --> lepton X0)/B(tau --> lepton nu nubar). Valid for mass(X0) < 100 MeV.  The limits rise to 7.1% (for mu), 5.0% (for e) for mass(X0) = 500 MeV.


pdgid: S029GB
text:
ATIYA 1990 limit is for mass(X0) = 0.  The limit B < 1E-8 holds for mass(X0) < 95 MeV. For the reduction of the limit due to finite lifetime of X0, see their Fig.3.


pdgid: S029GB
text:
BALKE 1988 limits are for B(mu+ --> e+ X0). Valid for mass(X0) < 80 MeV and  meanlife(X0) > E-8 sec.


pdgid: S029GB
text:
BOLTON 1988 limit corresponds to F > 3.1E9 GeV, which does not depend on the chirality property of the coupling.


pdgid: S029GB
text:
CHANDA 1988 find v_{{T}} < 10 MeV for the weak-triplet Higgs vacuum expectation value in Gelmini-Roncadelli model, and v_{{S}} > 5.8E6 GeV in the singlet Majoron model.


pdgid: S029GB
text:
CHOI 1988 used the observed neutrino flux from the supernova SN1987A to exclude the neutrino Majoron Yukawa coupling h in the range 2E-5 < h < 3E-4 for the interaction L(int) = 1/2ihpsibar(nu)**cgamma(5)psi_{{nu}}phi(X). For several families of neutrinos, the limit applies for (Sigmah(i)**4)**1/4.


pdgid: S029GB
text:
PICCIOTTO 1988 limit applies when mass(X0) < 55 MeV and meanlife(X0) > 2ns, and it decreases to 4E-7 at mass(X0) = 125 MeV, beyond which no limit is obtained.


pdgid: S029GB
text:
GOLDMAN 1987 limit corresponds to F > 2.9E9 GeV for the family symmetry breaking scale from the Lagrangian L(int) = (1/F)psibar_{{mu}}gamma**mu (a+bgamma_{{5}}) psi_{{e}}d(mu)phi(X0) with a**2+b**2 = 1. This is not as sensitive as the limit F >9.9E9 GeV derived from the search for mu+ --> e+ X0 by JODIDIO 1986, but does not depend on the chirality property of the coupling.


pdgid: S029GB
text:
Limits are for Gamma(mu --> e X0)/Gamma(mu --> e nu nubar). Valid when mass(X0) = 0-93.4, 98.1-103.5 MeV.


pdgid: S029GB
text:
EICHLER 1986 looked for mu+ --> e+ X0 followed by X0 --> e+ e-.  Limits on the branching fraction depend on the mass and and lifetime of X0.  The quoted limits are valid when meanlife(X0)~<3.E-10s if the decays are kinematically allowed.


pdgid: S029GB
text:
JODIDIO 1986 corresponds to F >9.9E9 GeV for the family symmetry breaking scale with the parity-conserving effective Lagrangian L(int) = (1/F) psibar_{{mu}}gamma**mupsi_{{e}}d**muphi(X0).


pdgid: S029GB
text:
BALTRUSAITIS 1985 search for light Goldstone boson(X0) of broken U(1). CL = 95% limits are B(tau --> mu+ X0)/B(tau --> mu+ nu nu) <0.125 and B(tau --> e+ X0)/B(tau --> e+ nu nu) <0.04.  Inferred limit for the symmetry breaking scale is m >3000 TeV.


pdgid: S029GB
text:
The primordial heavy neutrino must decay into nu and familon, f(A), early so that the red-shifted decay products are below critical density, see their table.  In addition, K --> pi f_A and mu --> e f_A are unseen.  Combining these excludes mass(heavy nu) between 5E-5 and 5E-4 MeV (mu decay) and mass(heavy nu) between 5E-5 and 0.1 MeV (K-decay).


pdgid: S029MT
text:
BERNATOWICZ 1992 studied double-beta decays of Te128 and Te130, and found the ratio tau(Te130)/tau(Te128) = 3.52+-0.11E-4 in agreement with relatively stable theoretical predictions.  The bound is based on the requirement that Majoron-emitting decay cannot be larger than the observed double-beta rate of Te128 of 7.7+-0.4E24 year. We calculated 90% CL limit as (7.7 -- 1.28x0.4=7.2)x10**24.


pdgid: S029MT
text:
AUGIER 2024 make 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 single Majoron mode of the 0nubeta beta decay of Mo100.  The range is due to the use of two different analysis strategies. Various limits on modes involving  the emission of multiple Majorons are given too. The derived range of constraints on the  Majoron-neutrino coupling constant is g(nu chi) < 4.0 -- 8.5E-5,  reflecting the variability of the used nuclear matrix elements and of the two data analysis  strategies.


pdgid: S029MT
text:
AZZOLINI 2023 use 9.95 kg.yr of data, collected by the CUPID-0 experiment, to place  a limit  on the single Majoron mode of the 0nubeta beta decay of Se82. Various  limits on  modes involving the emission of multiple Majorons are given too. The resulting  constraint on the  Majoron-neutrino coupling constant is g(nu chi) <  1.8 -- 4.4E-5. The  range is due to the variability of the used nuclear matrix elements.


pdgid: S029MT
text:
AGOSTINI 2022 use 32.8 kg.yr of GERDA phase 2 data to derive a limit of  g(nu chi) < 1.8 -- 4.4E-5 on the neutrino-Majoron coupling. The range  reflects the author's evaluation of the spread of nuclear matrix elements.


pdgid: S029MT
text:
AL-KHARUSI 2021 utilize the complete dataset of the EXO-200 experiment, corresponding to an  exposure of 234 kg yr, to place a limit on the one Majoron mode of the neutrinoless double beta  decay of Xe136. Several limits are reported, the one given here corresponds to a  spectral index of 1, resulting in a limit of g(nu chi)< 0.4 -- 0.9E-5  on the Majoron-neutrino coupling constant. The range reflects the spread of the nuclear matrix  elements.


pdgid: S029MT
text:
ARNOLD 2019 uses the NEMO-3 tracking calorimeter to determine limits for the Majoron emitting  double beta decay, with spectral index n = 3. The  limit corresponds to the range of the g_{{ee}}  coupling of 0.013 -- 0.035; dependimg on the nuclear matrix elements used.


pdgid: S029MT
text:
ARNOLD 2018 use the NEMO-3 tracking detector. The limit corresponds to <g_{{ee}}>  < 3.2 -- 8.0E-5; the range corresponds to different nuclear matrix element  calculations.


pdgid: S029MT
text:
AGOSTINI 2015A analyze a 20.3 kg yr of data set of the GERDA calorimeter to determine  g(nu chi)< 3.4 -- 8.7E-5 on the Majoron-neutrino  coupling constant.  The range reflects the spread of the nuclear matrix elements.


pdgid: S029MT
text:
ARNOLD 2015 use the NEMO-3 tracking calorimeter with 3.43 kg yr exposure to determine the  limit on Majoron emission. The limit corresponds to g(nu chi)< 1.6 -- 3.0E-4.  The spread reflects different nuclear matrix elements. Supersedes ARNOLD 2006.


pdgid: S029MT
text:
ALBERT 2014A utilize 100 kg yr of exposure of the EXO-200 tracking calorimeter to place a   limit on the g(nu chi)< 0.8 -- 1.7E-5 on the Majoron-neutrino   coupling constant. The range reflects the spread of the nuclear matrix elements.


pdgid: S029MT
text:
GANDO 2012 use the KamLAND-Zen detector to obtain the limit on the 0nuchi decay with Majoron emission.  It implies that the coupling constant g(nu chi)< 0.8 -- 1.6E-5 depending on the nuclear matrix elements used.


pdgid: S029MT
text:
ARNOLD 2011 use the NEMO-3 detector to obtain the reported limit on Majoron emission. It implies that the coupling constant g(nu chi) < 0.6 -- 1.6E-4 depending on the nuclear matrix element used. Supercedes ARNABOLDI 2003.


pdgid: S029MT
text:
ARGYRIADES 2010 use the NEMO-3 tracking detector and Zr96 to derive the reported limit. No limit for the Majoron electron coupling is given.


pdgid: S029MT
text:
ARGYRIADES 2009 use Nd150 data taken with the NEMO-3 tracking detector. The reported limit corresponds to < g(nu chi)>< 1.7 -- 3.0E-4 using a range of nuclear matrix elements that include the effect of nuclear deformation.


pdgid: S029MT
text:
ARNOLD 2006 use Mo100 data taken with the NEMO-3 tracking detector.  The reported limit corresponds to <g(nu chi)> < (0.4 -- 1.8)x10**-4  using a range of matrix element calculations. Superseded by ARNOLD 2015.


pdgid: S029MT
text:
NEMO-3 tracking calorimeter is used in ARNOLD 2006 . Reported half-life limit for Se82 corresponds to <g(nu chi)> < (0.66 -- 1.9)x10**-4 using a range of matrix element calculations. Supersedes ARNOLD 2004.


pdgid: S029MT
text:
ARNOLD 2004 use the NEMO-3 tracking detector. The limit corresponds to  <g(nu chi)> < (0.5 -- 0.9)10**-4 using the matrix elements  of SIMKOVIC 1999, STOICA 2001 and CIVITARESE 2003. Superseded by ARNOLD 2006.


pdgid: S029MT
text:
ARNOLD 2004 use the NEMO-3 tracking detector. The limit corresponds to <g(nu chi)> < (0.7 -- 1.6)10**-4 using the matrix elements of SIMKOVIC 1999, STOICA 2001 and CIVITARESE 2003.


pdgid: S029MT
text:
Supersedes ALESSANDRELLO 2000. Array of TeO(2) crystals in high resolution cryogenic calorimeter. Some enriched in Te130. Derive <g(nu chi)> < 17 -- 33E-5 depending on matrix element.


pdgid: S029MT
text:
Limit for the 0nu chi decay with Majoron emission of Cd116 using enriched CdWO(4) scintillators. <g(nu chi)><4.6 -- 8.1E-5 depending on the matrix element. Supersedes DANEVICH 2000.


pdgid: S029MT
text:
BERNABEI 2002D obtain limit for 0nu chi decay with Majoron emission of Xe136 using liquid Xe scintillation detector. They derive <g(nu chi)><2.0 -- 3.0E-5 with several nuclear matrix elements.


pdgid: S029MT
text:
Replaces TANAKA 1993. FUSHIMI 2002 derive half-life limit for the 0nu chidecay by means of tracking calorimeter ELEGANTV.  Considering various matrix element calculations, a range of limits for the Majoron-neutrino coupling is given: <g(nu chi)><(6.3 -- 360)x10**-5.


pdgid: S029MT
text:
DANEVICH 2001 obtain limit for the 0nu chi decay with Majoron emission of Gd160 using Gd(2)SiO(5):Ce crystal scintillators.


pdgid: S029MT
text:
ARNOLD 2000 reports limit for the 0nu chi decay with Majoron emission derived from tracking calorimeter NEMO2. Using Se82 source: <g(nu chi)><1.6E-4. Matrix element from GUENTHER 1996.


pdgid: S029MT
text:
ARNOLD 2000 reports limit for the 0nu 2chi decay with two Majoron emission derived from tracking calorimeter NEMO2.


pdgid: S029MT
text:
ARNOLD 1998 determine the limit for 0nu_{{chi}} decay with Majoron emission of Se82 using the NEMO-2 tracking detector. They derive <g(nu_{{chi}})> <2.3 -- 4.3E-4 with several nuclear matrix elements.


pdgid: S029MT
text:
LUESCHER 1998 report a limit for the 0nu decay with Majoron emission of Xe136 using Xe TPC.  This result is more stringent than BARABASH 1989. Using the matrix elements of ENGEL 1988, they obtain a limit on <g(nu chi)> of 2.0E-4.


pdgid: S029IAA
text:
BIANCHINI 2024 report a new limit on the axion mass, testing for the existence of a thermally  produced hot dark matter population using current cosmic microwave background and baryon acoustic  oscillation data. This analysis presents a stronger limit than previous bounds, e.g. NOTARI 2023.


pdgid: S029IAA
text:
CHENG 2023 employ an improved approximation of the boson cloud eigenfrequency to calculate   the superradiance rate. They find that sensitivity depends on initial spin distribution and the   merger timescale, and identify two preferred ranges for boson mass centered at 1.78E-12 and   7.94E-13 eV.


pdgid: S029IAA
text:
DELLA-MONICA 2023 consider the solitonic core implied by ultralight scalar dark matter in the  centre of the Milky Way and the effect its presence would have on the precisely tracked orbits of  the stars orbiting our galaxy's central supermassive black hole, Sagittarius A***.


pdgid: S029IAA
text:
DERBIN 2023 employ a thulium garnet crystal bolometer to search for the 8.4 keV solar axion  line emitted from the M1 nuclear transition of thulium-169, Tm169. Mass bound applies to  KSVZ axions, value for DFSZ is 244 eV.


pdgid: S029IAA
text:
NOTARI 2023 improved the evaluation of axion production from pion scatterings by using   pion-pion scattering data and incorporating the momentum dependence of the Boltzmann equation. The   limit is based on the Planck 2018, BAO, and Pantheon SN Ia data.


pdgid: S029IAA
text:
ROGERS 2023 use the CMB and BOSS galaxy-clustering data to set limits on the abundance of  ultralight axion DM. They obtained Omega(A0) < 0.002 for mass(A0) =  E-30 -- E-28 eV and set upper limits ranging from 0.002 to 0.07 for mass(A0) = E-32 -- E-25  eV. See their Fig. 22 for mass-dependent limits.


pdgid: S029IAA
text:
SMARRA 2023 is the European Pulsar Timing Array's constraint on the contribution of  ultralight DM to the DM density in our local galactic neighbourhood. Ultralight DM cannot saturate  the known DM density of 0.3 GeV/cc for masses inside this mass interval of E-24 -- 5E-23 eV.


pdgid: S029IAA
text:
XIA 2023 is analogous to PORAYKO 2018 and use the Fermi-LAT pulsar timing array. They   set a bound on the local density as rho(A0) ~< 8 GeV/cm**3 for mass(A0)   ~< E-23 eV at 95% CL, with weaker constraints up to E-22 eV. See their Fig. 1  for the mass-dependent limits.


pdgid: S029IAA
text:
LAGUE 2022 used the BOSS galaxy-clustering data to set limits on the abundance of ultralight   axion dark matter. When combined with the CMB data, they obtained   Omega(A0)h**2 < 0.004 for mass(A0) = E-31 -- E-26 eV.   See their Figs. 1 and 15 for mass-dependent limits.


pdgid: S029IAA
text:
YUAN 2022A use the data of Advanced LIGO and Advanced Virgo's first three observing runs to  search for stochastic GW background produced by scalar bosonic clouds formed by the BH superradiant  instability. They set the limit, taking into account all the unstable modes.


pdgid: S029IAA
text:
BANIK 2021 use the subhalo mass function inferred from the analyses of the GD-1 and Pal 5  stellar streams. The limit is strengthened to 2.2E-21 eV when adding dwarf satellite counts.


pdgid: S029IAA
text:
BAUMHOLZER 2021 study the freeze-in production of axion dark matter through couplings to  photons, and set the limit using Lyman-alpha forest data and the observed number of Milky  Way subhalos.


pdgid: S029IAA
text:
CROON 2021 study the supernova cooling effect of the axion-muon coupling, taking account of  semi-Compton scattering and muon-proton bremsstrahlung, as well as the loop-induced axion-photon  coupling, and exclude the range of g(A mu mu) ~= 7E-3 -- 2E-10 for  mass(A0) < 0.5 GeV. See their Fig. 8 for mass-dependent limits.


pdgid: S029IAA
text:
FUJIKURA 2021 use the EROS-2 survey and the Subaru HSC observation to set limits on  spherically symmetric axion clumps, taking account of the finite lens and source size effects.  f(A0) ~> E12 GeV can be constrained depending on the fraction of the  axion dark matter collapsed into clumps, and the clump densities. See their Figs. 7 -- 10  for the limits.


pdgid: S029IAA
text:
MARTINCAMALICH 2021 considered axion emission from a supernova core through the Lambda   hyperon  decay, and set the limit on B(Lambda --> n A0) ~< 8E-9, or equivalently,    f(A0)/C(sd) ~> 2.6E9 GeV in terms of the flavor-violating axion    coupling to the down and strange quarks.


pdgid: S029IAA
text:
NG 2021 use the binary black holes reported by LIGO and Virgo to determine the black hole  spin distribution at formation and the scalar boson mass simultaneously, neglecting the boson  self-interaction.


pdgid: S029IAA
text:
ROGERS 2021 set the limit by using a framework involving Bayesian emulator optimization to  accurately forward-model the Lyman-alpha flux power spectrum, and comparing this with  small-scale data to constrain the predicted suppression of cosmic structure growth.


pdgid: S029IAA
text:
TSUKADA 2021 look for a stochastic GW background produced by extragalactic BH-hidden photon   cloud systems through the superradiant instability. They assume a uniform spin distribution at  birth of isolated BHs from 0 to 1.


pdgid: S029IAA
text:
IRSIC 2020 used the Lyman-alpha forest constraint on small-scale isocurvature  perturbation to derive limits on the axion mass and decay constant, assuming that the axion makes  up all dark matter in the post-inflationary scenario. See their Fig. 1 for other astrophysical  limits as well as the limits on the case of the temperature-dependent axion mass.


pdgid: S029IAA
text:
PODDAR 2020 used the observed decay in orbital period of four compact binary systems to  derive a limit on the emission of axions with mass(A0) < 1E-19 eV, assuming they couple  to nucleons and the strong CP phase vanishes at the potential minimum. They exclude  f(A0) ~< E11 GeV for such axions.


pdgid: S029IAA
text:
SCHUTZ 2020 set a limit on fuzzy dark matter based on the existing limits for warm dark  matter derived from the inferred subhalo mass function.


pdgid: S029IAA
text:
SUN 2020 look for quasimonochromatic gravitational waves emitted from boson clouds around the  Cygnus X-1 black hole. The quoted limit assume the black hole age of 5E6 years. A mass range of  9.6 -- 15.5E-13 eV is disfavored when repeated induction of bosenova for string axions with  decay constant f(A0) ~= E15 GeV prevents the superradiance from being  saturated.


pdgid: S029IAA
text:
DAVOUDIASL 2019 used the observed data of M87* by the Event Horizon Telescope to set the  limit. A mass range of 0.85 -- 4.6E-21 eV is disfavored for a spin-1 boson.


pdgid: S029IAA
text:
MARSH 2019 considered heating of star clusters due to the stochastic oscillations of the core  and granular quasiparticles in the outer halo. The limit was derived by requiring the survival of  the old star cluster in Eridanus II, where the lower end is set by the validity of diffusion  approximation. The effect of tidal stripping is also discussed for lower masses.


pdgid: S029IAA
text:
PALOMBA 2019 used the LIGO O2 dataset to derive limits on nearly monochromatic gravitational  waves emitted by boson clouds formed around a stellar-mass black hole. They exclude boson masses in  a range of 1.1E-13 and 4E-13 eV for high initial black hole spin, and 1.2E-13 and  1.8E-13 eV for moderate spin. See their Figs. 2 and 3 for limits based on various values of  black hole initial spin, boson cloud age, and distance.


pdgid: S029IAA
text:
CHANG 2018 update axion bremsstrahlung emission rates in nucleon-nucleon collisions, shifting  the excluded mass range to higher values. They rule out the hadronic axion with mass up to a few  hundred eV, closing the hadronic axion window. See their Fig. 11 for results based on several  different choices of the temperature and density profile of the proto-neutron star.


pdgid: S029IAA
text:
PORAYKO 2018 look for time-dependent oscillations in the gravitational potential generated by   ultralight scalar dark matter, and set a bound on its local density as rho(A0)   ~< 6 GeV/cm**3 for mass(A0) ~< E-23 eV at 95% CL. See their Fig. 4 for  the limits.


pdgid: S029IAA
text:
ARCHIDIACONO 2013A is analogous to HANNESTAD 2005A. The limit is based on the CMB temperature power spectrum of the Planck data, the CMB polarization from the WMAP 9-yr data, the matter power spectrum from SDSS-DR7, and the local Hubble parameter measurement by the Carnegie Hubble program.


pdgid: S029IAA
text:
CADAMURO 2011 use the deuterium abundance to show that the mass(A0) range 0.7eV -- 300keV is excluded for axions, complementing HANNESTAD 2010.


pdgid: S029IAA
text:
DERBIN 2011A look for solar axions produced by Compton and bremsstrahlung processes, in the resonant excitation of Tm169, constraining the axion-electron x axion nucleon couplings.


pdgid: S029IAA
text:
ANDRIAMONJE 2010 search for solar axions produced from Li7  (478 keV) and D(p,gamma)He3 (5.5 MeV) nuclear transitions. They show limits on the axion-photon coupling for two reference values of  the axion-nucleon coupling for mass(A)< 100 eV.


pdgid: S029IAA
text:
ANDRIAMONJE 2009 look for solar axions produced from the thermally excited 14.4 keV level of Fe57. They show limits on the axion-nucleon x axion-photon coupling assuming mass(A)< 0.03 eV.


pdgid: S029IAA
text:
DERBIN 2009A look for Primakoff-produced solar axions in the resonant excitation of Tm169, constraining the axion-photon x axion-nucleon couplings.


pdgid: S029IAA
text:
KEKEZ 2009 look at axio-electric effect of solar axions in HPGe detectors.  The one-loop axion-electron coupling for hadronic axions is used.


pdgid: S029IAA
text:
This is an update of HANNESTAD 2005A with new cosmological data, notably WMAP (3 years) and baryon acoustic oscillations (BAO). Lyman-alpha data are left out, in contrast to HANNESTAD 2005A and MELCHIORRI 2007A, because it is argued that systematic errors are large. It uses Bayesian statistics and marginalizes over a possible neutrino hot dark matter component.


pdgid: S029IAA
text:
MELCHIORRI 2007A is analogous to HANNESTAD 2005A, with updated cosmological data, notably WMAP (3 years). Uses Bayesian statistics and marginalizes over a possible neutrino hot dark matter component. Leaving out Lyman-alpha data, a conservative limit is 1.4 eV.


pdgid: S029IAA
text:
HANNESTAD 2005A puts an upper limit on the mass of hadronic axion because in this mass range it would have been thermalized and contribute to the hot dark matter component of the universe. The limit is based on the CMB anisotropy from WMAP, SDSS large scale structure, Lyman alpha, and the prior Hubble parameter from HST Key Project. A chi^2 statistic is used. Neutrinos are assumed not to contribute to hot dark matter.


pdgid: S029IAA
text:
MOROI 1998 points out that a KSVZ axion of this mass range (see CHANG 1993) can be a viable hot dark matter of Universe, as long as the model-dependent g(A gamma) is accidentally small enough as originally emphasized by KAPLAN 1985; see Fig.1.


pdgid: S029IAA
text:
BORISOV 1997 bound is on the axion-electron coupling g(ae)<1E-13 from the photo-production of axions off of magnetic fields in the outer layers of neutron stars.


pdgid: S029IAA
text:
KACHELRIESS 1997 bound is on the axion-electron coupling g(ae)<1E-10 from the production of axions in strongly magnetized neutron stars.  The authors also quote a stronger limit, g(ae)<9E-13 which is strongly dependent on the strength of the magnetic field in white dwarfs.


pdgid: S029IAA
text:
KEIL 1997 uses new measurements of the axial-vector coupling strength of nucleons, as well as a reanalysis of many-body effects and pion-emission processes in the core of the neutron star, to update limits on the invisible-axion mass.


pdgid: S029IAA
text:
RAFFELT 1995 reexamined the constraints on axion emission from red giants due to the axion-electron coupling.  They improve on DEARBORN 1986 by taking into proper account degeneracy effects in the bremsstrahlung rate. The limit comes from requiring the red giant core mass at helium ignition not to exceed its standard value by more than 5% (0.025 solar masses).


pdgid: S029IAA
text:
ALTHERR 1994 bound is on the axion-electron coupling g(ae)<1.5E-13, from energy loss via axion emission.


pdgid: S029IAA
text:
CHANG 1993 updates ENGEL 1990 bound with the Kaplan-Manohar ambiguity in z=mass(u)/mass(d) (see the Note on the Quark Masses in the Quark Particle Listings).  It leaves the window f(A)=3E5-3E6 GeV open. The constraint from Big-Bang Nucleosynthesis is satisfied in this window as well.


pdgid: S029IAA
text:
BERSHADY 1991 searched for a line at wave length from 3100 -- 8300 angstroms expected from 2gamma decays of relic thermal axions in intergalactic light of three rich clusters of galaxies.


pdgid: S029IAA
text:
KIM 1991C argues that the bound from the mass density of the universe will change drastically for the supersymmetric models due to the entropy production of saxion (scalar component in the axionic chiral multiplet) decay.  Note that it is an upperbound rather than a lowerbound.


pdgid: S029IAA
text:
RAFFELT 1991B argue that previous SN1987A bounds must be relaxed due to corrections to nucleon bremsstrahlung processes.


pdgid: S029IAA
text:
ENGEL 1990 rule out 10**-10~< g(AN) ~<10**-3, which for a hadronic axion with EMC motivated axion-nucleon couplings corresponds to 2.5E-3eV ~< mass(A0) ~< 2.5E4eV.  The constraint is loose in the middle of the range, i.e. for electron gfactor(AN) ~10**-6.


pdgid: S029IAA
text:
ERICSON 1989 considered various nuclear corrections to axion emission in a supernova core, and found a reduction of the previous limit (MAYLE 1988) by a large factor.


pdgid: S029IAA
text:
MAYLE 1989 limit based on naive quark model couplings of axion to nucleons.  Limit based on couplings motivated by EMC measurements is 2-4 times weaker.  The limit from axion-electron coupling is weak: see HATSUDA 1988B.


pdgid: S029IAA
text:
RAFFELT 1988B derives a limit for the energy generation rate by exotic processes in helium-burning stars epsilon < 100 erg g**-1 s**-1, which gives a firmer basis for the axion limits based on red giant cooling.


pdgid: S029IAA
text:
RAFFELT 1986 gives a limit electron gfactor(Agamma) < 1.1E-10 GeV**-1 from red giants and <2.4E-9 GeV**-1 from the sun.


pdgid: S029AXI
text:
AHN 2024 is from the CAPP-MAX experiment with sensitivity to DFSZ axions. See Fig. 22 for  mass-dependent limits.


pdgid: S029AXI
text:
BAE 2024 search for dark matter axions using a microwave cavity with a tunable TM020 mode,  scanning around 5 GHz. See their Fig. 6 for mass-dependent limits.


pdgid: S029AXI
text:
DAVYDOV 2024 constrain ultralight axion-like particle dark matter via the oscillating  birefringence effect induced by the local ALP field. Their constraint is based on polarimetric  measurements of the HL Tauri protoplanetary disk. Their constraint is g(a gamma)  < 2.111E-12 GeV**-1(mass(a)/E-22) eV.


pdgid: S029AXI
text:
HEINZE 2024 search for ALP dark matter using the LIDA experiment - a laser interferometric  haloscope that can detect the axion-induced polarisation rotation of light. Quoted limit assumes a  dark matter density of 0.4 GeV/cm**3. See their Fig. 2 for mass-dependent limits.


pdgid: S029AXI
text:
KIM 2024 report results from the CAPP-12T experiment searching for dark matter axions around  22 mueV down to the KSVZ level. See their Fig. 5 for mass-dependent limits.


pdgid: S029AXI
text:
PANDEY 2024 report first search from the ADBC haloscope - an optical bow-tie laser cavity  searching for the oscillating birefringence effect due to axion dark matter coupled to the photon.  See their Fig. 3 for mass-dependent limits.


pdgid: S029AXI
text:
QUISKAMP 2024 present results from Phase 1b of the ORGAN experiment, a high-frequency  resonant axion haloscope in the 15 -- 50 GHz range. See their Fig. 5 for mass-dependent  limits.


pdgid: S029AXI
text:
RETTAROLI 2024 report results from the QUAX resonant cavity haloscope at 8.8 GHz. This  extends their previous search around this mass range reported in ALESINI 2019. See their Fig.  7 for mass-dependent limits.


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ADACHI 2023D is analogous to ADE 2021. They used POLARBEAR data, and take account of a  stochastic local axion field amplitude with the time-averaged local axion density rho_{{A}} = 0.3  GeV/cm**3. Limits are set at G(A gamma gamma) < 2.4E-11 GeV**-1  (mass(A0)/E-21 eV), which is 2.2 times larger than the deterministic case. See Fig. 5 for  mass-dependent limits.


pdgid: S029AXI
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DI-VORA 2023 searches for axions in a narrow mass window using an 8T haloscope and a  travelling wave parametric amplifier to achieve noise close to the quantum limit. This is an  improvement on their previous scan at the same mass, ALESINI 2021. See Fig. 7 for  mass-dependent limits and a comparison.


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JEWELL 2023 correct an underestimation of intermediate frequency noise in BACKES 2021.  See their Fig. 11 for the mass-dependent limits.


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KIM 2023 is an update of KWON 2021 on the CAPP-PACE experiment.  See their Fig. 4 for  mass-dependent limits.


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OSHIMA 2023 report first limits from the DANCE experiment. This experiment is based on a  novel bow-tie cavity design that searches for the oscillating rotation of polarised laser light  driven by the DM axion-photon mixing at low frequencies. See their Fig. 6 for mass-dependent limits.


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THOMSON 2023 used an AC microwave cavity to search for dark matter axions. The axion signal  is resonantly enhanced when the axion mass matches the difference between a cavity which is pumped  with power and another resonant mode close in frequency that is used to read out the signal. See  their Fig. 7 for the mass-dependent limits.


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YANG 2023 extends the first phase of CAPP 18T to KSVZ axions between 4.8077 and 4.8181 GHz.  They used an 18T high-temperature superconducting magnet haloscope. See their Fig. 5 for  mass-dependent limits. Quoted value is for their limit derived with a Bayesian method.


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YI 2023 is analogous to LEE 2020A, using the CAPP-12TB haloscope. See their Fig. 4 for  mass-dependent limits.


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YI 2023A used the same data as YI 2023, but instead of the standard halo model, they  searched for axion dark matter in the Sagittarius tidal stream with a velocity v = 300  km/sec and a velocity dispersion deltav = 20 km/sec. See their Fig. 4 for  mass-dependent limits.


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ADE 2022 is an update of ADE 2021 based on the expanded data of the 2012 -- 2015   observing seasons. See their Fig. 3 for mass-dependent limits over the extended mass range  1E-23 -- 6E-19 eV.


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ALESINI 2022 is an update of ALESINI 2021, using the TM030 mode of the cylindrical  dielectric cavity. See their Fig. 8 for mass-dependent limits.


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BATTYE 2022 is analogous to DARLING 2020A, and use plasma ray tracing technique to  analyze the propagation of radio photons converted from axion dark matter in the magnetosphere of  PSR J1745-2900. The quoted limit assumes rho_{{A}} = 6.5E4 GeV/cm**3 in the vicinity of  the magnetar. See their Fig. 1 for mass-dependent limits.


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CHANG 2022 used a microwave cavity detector to search for dark matter axions. See Fig. 3 for  the mass-dependent limits.


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FERGUSON 2022 is analogous to ADE 2021. They use the data of the SPT-3G's 2019    observing season. See their Fig. 5 for mass-dependent limits over the extended mass range    0.047 -- 9.5E-20 eV.


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LEE 2022 is analogous to LEE 2020A. They used an 18T high-temperature superconducting  magnet haloscope. See their Fig. 5 for mass-dependent limits.


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QUISKAMP 2022 is a 15.28 to 16.23 GHz microwave cavity haloscope with 11.5 T B-field. See   Fig. 4  for mass-dependent limits.


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YOON 2022 analyzed the data from LEE 2022 and changed from a frequentist to a  Bayesian  method to set limits. See their Fig. 27 for mass-dependent limits.


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ZHOU 2022 is analogous to DARLING 2020A, and they use the data from the MeerKAT radio  telescope's observation of the neutron star J0806.4-4123, which is 250 pc from Earth. See their  Fig.3 for mass-dependent limits.


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ADE 2021 looks for a time-variable global rotation of the CMB polarization induced by the   harmonic oscillations of local axion-like dark matter and uses data from the 2012 observing season  of the Keck Array, part of the BICEP program. The limits get 25% weaker for mass(A0) =   4.8E-20 -- 5.7E-19 eV. See their Eq. (80) and Fig. 6 for mass-dependent limits.


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DEVLIN 2021 use the superconducting resonant detection circuit of a cryogenic Penning trap  with a single antiproton. See their Fig. 3 for mass-dependent limits.


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GRAMOLIN 2021 use two detection channels, each consisting of two stacked toroids to look for  the axion-induced oscillating magnetic field. The quoted limit applies at mass(A0) = 0.02 neV. See  their Fig. 4 for mass-dependent limits.


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KWON 2021 is analogous to LEE 2020A. They also obtain weaker limits in the range of   mass(A0) = 10.16 -- 11.37 mueV. See their Fig. 4 for mass-dependent limits.


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MELCON 2021 use a radio frequency cavity consisting of 5 sub-cavities coupled by inductive  irises installed inside the CAST dipole magnet to look for higher axion masses. See their Fig. 9  for mass-dependent limits.


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THOMSON 2021 use a resonant cavity supporting two spatially overlapping microwave modes,  which is sensitive to the axion mass corresponding to the sum or difference of the two resonant  frequencies. The original limit was retracted due to a sign error. See their Fig. 2 in the erratum  for the corrected limits.


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YUAN 2021 use polarimetric observations of Sgr A***  taken by the Event Horizon Telescope  to search for periodic oscillation of the polarization induced by axion dark matter, assuming a  solitonic core near the Galactic center. They obtained limits in the range of G(A gamma gamma) =  8E-13 -- 3E-11 GeV**-1.


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CRISOSTO 2020 used a resonant LC circuit to look for lighter axion dark matter. They obtained  a similar, slightly weaker limit for mass(A0) = 174.98 -- 175.19 and 177.34 -- 177.38 neV. See  their Fig. 4 for mass-dependent limits.


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DARLING 2020A use VLA data to look for radio-frequency radiation converted from axion dark  matter in the magnetosphere of the Galactic Center magnetar PSR J1745-2900. They extended the  results of DARLING 2020, which used only data with the highest angular resolution, by adding  sub-optimal data. They use rho_{{A}} = 6.5E4 GeV/cm**3 in the vicinity of the magnetar.  See their Fig. 2 for mass-dependent limits.


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FOSTER 2020 look for radio-frequency radiation converted from axion dark matter in the  magnetic field around neutron stars. They use the observed data of isolated local neutron stars and  in the Galactic center. The quoted limit applies to mass(A0) ~= 7 mueV. See their  Fig. 2 for mass-dependent limits.


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JEONG 2020 is analogous to LEE 2020A, and they use a double-cell cavity to look for  axions with mass > 10 mueV. See their Fig. 5 for mass-dependent limits.


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KENNEDY 2020 is analogous to BRANCA 2017, and they compare the frequency ratios of the  Si cavity measured by a Sr optical lattice clock and by a H maser.  Assuming the local density of moduli dark matter, rho(S) = 0.3 GeV/cm**3, they  obtain a limit G(S gamma gamma) < 5.8E-24 GeV**-1 at mass(S0) =  2E-19 eV.  See their Fig. 2 for mass-dependent limits as well as limits on the modulus coupling  to electrons.


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LEE 2020A used a microwave cavity detector at the IBS/CAPP to search for dark matter axions.  See Fig. 3 for the mass-dependent limits.


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ALESINI 2019 used a superconducting resonant cavity made of NbTi to increase the  quality factor. The limit applies to a mass range of 0.2 neV around mass(A0) = 37.5 mueV.


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FUJITA 2019 look for photon birefringence under the oscillating axion background using the  polarimetric imaging observation of a protoplanetary disk, AB Aur. See their Fig. 2 for a more  conservative limit taking account of possible systematic effects.


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OUELLET 2019A look for the axion-induced oscillating magnetic field generated by a toroidal  magnetic field. The quoted limit applies at mass(A0) = 8 neV. See their Fig. 3 for the  mass-dependent limits.


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BOUTAN 2018 use a small high frequency cavity installed above the main ADMX cavity to look  for heavier axion dark matter. See their Fig. 4 for mass-dependent limits.


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DU 2018 is analogous to DUFFY 2006. They upgraded a dilution refrigerator to reduce the  system noise. The quoted limit is around mass(A0) = 2.69 mueV  for the boosted Maxwellian  axion line shape. See Fig. 4 for their mass-dependent limits.


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ZHONG 2018 is analogous to BRUBAKER 2017.  The quoted limit applies at mass(A0) =  23.76 mueV. See Fig. 4 for their mass-dependent limits.


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BRANCA 2017 look for modulations of the fine-structure constant and the electron mass due to  moduli dark matter by using the cryogenic resonant-mass AURIGA detector.  The limit on the assumed  dilatonic coupling implies G(S gamma gamma) < 1.5E-24 GeV**-1 for  the scalar to two-photon coupling. See Fig. 5 for the mass-dependent limits.


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BRUBAKER 2017 used a microwave cavity detector at the Yale Wright Laboratory to search for  dark matter axions. See Fig. 3 for the mass-dependent limits.


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CHOI 2017 used a microwave cavity detector with toroidal geometry. See Fig. 4 for their  mass-dependent limits.


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MCALLISTER 2017 used a high-frequency microwave cavity haloscope at 26.6 GHz in a 7 T   magnetic field. See Fig. 4 for mass-dependent limits.


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HOSKINS 2016 is analogous to DUFFY 2006. See Fig.12 for mass-dependent limits  in terms of the local dark matter density.


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BECK 2013 argues that dark-matter axions passing through Earth may generate a small observable signal in resonant S/N/S Josephson junctions. A measurement by HOFFMANN 2004 [Physical Review  B70 180503 (2004)] is interpreted in terms of subdominant dark matter axions with mass(A0) = 0.11 meV.


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HOSKINS 2011 is analogous to DUFFY 2006. See Fig.4 for the mass-dependent limit in terms of the local density.


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ASZTALOS 2010 used the upgraded detector of ASZTALOS 2004 to search for halo axions. See their Fig.5 for the mass(A0) dependence of the limit.


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DUFFY 2006 used the upgraded detector of ASZTALOS 2004, while assuming a smaller velocity dispersion than the isothermal model as in Eq. (8) of their paper. See Fig. 10 of their paper on the axion mass dependence of the limit.


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ASZTALOS 2004 looked for a conversion of halo axions to microwave photons in magnetic field. At 90% CL, the KSVZ axion cannot have a local halo density more than 0.45~GeV/cm**3 in the quoted mass range.  See Fig.~7 of their paper on the axion mass dependence of the limit.


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KIM 1998 calculated the axion-to-photon couplings for various axion models and compared them to the HAGMANN 1990 bounds.  This analysis demonstrates a strong model dependence of G(A gamma gamma) and hence the bound from relic axion search.


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WUENSCH 1989 looks for condensed axions near the earth that could be converted to photons in the presence of an intense electromagnetic field via the Primakoff effect, following the proposal of SIKIVIE 1983.  The theoretical prediction with [G(A gamma gamma)/mass(A0)]**2 = 2E-14 MeV**-4 (the three generation DFSZ model) and rho(A) = 300 MeV/cm**3 that makes up galactic halos gives (G(A gamma gamma)/mass(A0))**2 rho(A) = 4E-44. Note that our definition of G(A gamma gamma) is (1/4pi) smaller than that of WUENSCH 1989.


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ABLIKIM 2024AD constrain the axion-photon coupling through radiative J/psi decays in the  BESIII detector at the Beijing electron-positron collider. See their Fig. 5 for mass-dependent  limits.


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ALTENMULLER 2024 report an extended search for solar axions using the CAST experiment. The  experiment employed a new xenon-based microMEGAS detector - a pathfinder for the future  International Axion Observatory (IAXO). This limit improves upon ANASTASSOPOULOS 2017. See  Fig. 4 for mass-dependent limits.


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DEV 2024 use Fermi gamma-ray observations of the neutron star merger GW170817 to constrain  the production and subsequent decay of high-mass axion-like particles. Constraint extends  diagonally in mass-coupling space, reaching 7E-12 GeV**-1 at 100 MeV. See Fig. 4 for  mass-dependent limits.


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DIAMOND 2024 use multi-messenger observations of the neutron star merger GW170817 to  constrain the production and radiative decay of axions in the event. Limits shown in their Fig. 3  extend diagonally in mass-coupling space.


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FORDHAM 2024 use asteroseismology observations of a solar-like star, KIC 6933899, to  constrain axion emission from its interior via the photon coupling. Bound applies to all axion  masses up to around the core temperature of the star ~keV.


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GAO 2024 constrain ALP-photon oscillations via their imprint on the gamma-ray spectrum of the  blazar Mrk 421, as observed by MAGIC and Fermi-LAT. See their Fig. 5 for mass-dependent limits.


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GAO 2024A constrain ALP-photon oscillations using the high-energy gamma-ray spectrum observed  by LHAASO of the brightest gamma-ray burst so far detected, GRB 221009A. See their Fig. 5 for  mass-dependent limits. The strength of the limit depends on the magnetic field of the host galaxy.


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GUO 2024 search for axion dark matter decaying or converting into photons in the Coma  Berenices dwarf galaxy using the radio telescope FAST. The quoted limit is for the case of axions  decaying, including stimulated emission. See their Fig. 2 for mass-dependent limits.


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LI 2024A constrain the imprint of ALP-photon oscillations on the TeV gamma-ray spectrum of  the BL Lac blazar 1ES 1215+303 using VERITAS and Fermi-LAT data. See their Fig. 4 for  mass-dependent limits.


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LI 2024B constrain the imprint of ALP-photon oscillations on the very-high-energy gamma-ray  spectrum of various galactic sources detected by the LHAASO air-shower array. Best limits are  obtained from the Crab Nebula after combining several observations from different gamma-ray  observatories in addition to LHAASO. See their Fig. 5 for mass-dependent limits.


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LI 2024D search for evidence of axion-photon oscillations imprinted on the gamma-ray spectrum  of the nearby BL Lac blazar Markarian 421. They set upper limits using data from Fermi-LAT and  HAWC. The quoted limit applies for mass(A0) ~= 3E-9 eV. See their Fig. 3 for  mass-dependent limits.


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MANZARI 2024 search for evidence of axions produced in SN1987A converting into gamma-rays  that would have been detectable by the Solar Maximum Mission. This analysis improves upon previous  studies of axion-photon conversion after SN1987A (e.g. HOOF 2023) by including the magnetic  field of the progenitor star. Quoted limit applies for masses below  0.1 neV and rises towards  larger masses. See their Fig. 1 for mass-dependent limits.


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PANT 2024 searches for the imprint of axion-photon oscillations in the very-high-energy  gamma-ray spectrum of the quasar QSO B1420+326 observed by the MAGIC telescope. Three small  disconnected regions of mass-coupling parameter space below 1 neV are ruled out. See Fig. 4 for the  limits.


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PYBUS 2024 report results from the GlueX detector, which has searched for the two-photon  decay of heavy axions produced through the nuclear Primakoff effect due to a beam of photons  incident on a Carbon target. See their Fig. 8 for mass-dependent limits.


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RAVENSBURG 2024 search for heavy axions decaying to two photons using the recent nearby  type-II supernova SN 2023ixf. Constraint extends diagonally downwards in mass-coupling space, see  their Fig. 2 for full limits. Quoted limit is the most constraining point for the most conservative  choices for supernova parameters.


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TODARELLO 2024 search for axions decaying to two photons in the halos of Milky Way dwarf  galaxies observed in the MUSE-Faint survey. This study improves upon an earlier one presented in  REGIS 2021. See their Fig. 5 for compiled mass-dependent limits.


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WANG 2024A search for axions decaying into two photons assuming that they make up the dark  matter halos of galaxies. They use data from the Dark Energy Spectroscopic Instrument, searching  for the axion decay line in optical wavelengths with their Bright Galaxy and Luminous Red Galaxy  samples. See their Fig. 8 for mass-dependent limits on the axion to photon decay rate. Their  constraint is quoted as a 5sigma detection limit.


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BATTYE 2023 look for dark-matter axions falling into pulsar magnetospheres and converting  into narrow radio lines. Unlike the earlier FOSTER 2022 they search for evidence of  conversion in the time-domain signal of a single pulsar, using 1 hour of MeerKAT data on the pulsar  PSR J2144-3933. The quoted limit applies to an assumed magnetic field of 2E12 G and a dark  matter density of 0.45 GeV/cm**3.


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BEAUFORT 2023 extends DEROCCO 2022 who searched for the X-ray decay of axions that  build up in the gravitational well of the Sun over its lifetime, the 'solar basin'. They use data  from NuSTAR and SphinX telescopes and extends the previous study by accounting for the axion  production via photon coalescence.


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BERNAL 2023 use gamma-ray data from 739 blazars observed by FermiLAT and 38 blazars by  Cherenkov observatories. They estimate optical depth, subtract the astrophysical component, and  attribute the residual to axion two-photon decay. The quoted limit is for mass(A0) ~= 25 eV.  See their Fig. 3 for the mass-dependent limits.


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CAPOZZI 2023 use Planck CMB and Lyman-alpha observations to set limits on early  energy injection by decaying dark matter axions that would affect CMB anisotropies and the  reionisation history of the Universe. The quoted limit applies to mass(A0) = 100 eV and the  reionization model of Fauchere-Giguere. See Fig. 4 for mass-dependent constraints from different  reionization models.


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CAPOZZI 2023A search for axions produced in electromagnetic showers in proton beam dumps and  fixed target experiments. In this case, they reinterpret MiniBoone data. Quoted limit applies at  100 MeV but the limit does not extend to arbitrarily large couplings. See Fig. 7 for mass-dependent  limits.


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DAVIES 2023 is analogous to AJELLO 2016, and use the Fermi-LAT data from three quasars  (3C454.3, CTA 102, and 3C279), considering the blazer jets as the regions where the axion-photon  oscillations occur. See Fig. 8 for the mass-dependent limits.


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DIAMOND 2023 demonstrate that a window of decaying 10-MeV-mass ALP parameter space previously  thought to be excluded by the lack of gamma-ray emission from the SN 1987A explosion is actually  unconstrained because of the formation of a fireball that would prevent decay photons from  escaping. They nevertheless re-exclude this window by considering the non-detection of the sub-MeV  emission by the Pioneer Venus Orbiter. The quoted limit is at mass(A0) = 56 MeV. See their Fig. 2  for mass-dependent limits.


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FILZINGER 2023 searched for oscillations in the fine structure constant induced by   dilaton-like dark matter by measuring the frequency ratio between the E3 and E2 transitions of   Yb171**+. They assume the local dark matter density  rho_{{S}} = 0.4 GeV/cm**3.   The quoted limit is set at mass(S0) ~= 4E-23 eV. See their Fig. 4 for the limits over  mass(S0) = 1E-24 -- 1E-17 eV.


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HOOF 2023 consider axions emitted from SN1987A converting to gamma rays in Galactic magnetic    fields, using temporal information of the Solar Maximum Mission data. They set a limit    G(A gamma gamma) ~< 5E-12 for masses mass(A0) ~< 2E-10 eV.  See left panel in Fig. 3 for mass-dependent limits.


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HOOF 2023 look for gamma rays resulting from the decay of axions produced from SN1987A, using  the  Solar Maximum Mission data. See right panel in Fig. 3 for mass-dependent limits.


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JACOBSEN 2023 search for the imprints of axion-photon mixing on the TeV spectra of several  blazars using data from the HAWC air shower detector.


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LI 2023H look for gamma-ray spectral irregularities induced by axion-photon oscillations from   AGN VER J0521+211, using the Fermi-LAT and VERITAS data. See their Fig. 4 for mass-dependent  limits.


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NOORDHUIS 2023 places strong constraints on the axion-photon coupling over a broad mass  window using the fact that the polar cap regions of pulsars can generate a population of axions,  which would then convert into an observable outgoing radio flux in the presence of the neutron  star's B-field. They search for this signal in 27 pulsars and set mass-dependent limits shown in  their Fig. 2.


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PANT 2023 study the effect of axion-photon oscillations on the gamma-ray spectrum   from the  extragalactic neutrino source, TXS 0506+056. The quoted limit is at mass(A0) ~=   2.7E-7  eV.  See their Fig. 2 for mass-dependent limits.


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SHERRILL 2023 search for scalar dilaton-like dark matter via oscillations in the fundamental  constants. Their most competitive constraint is on the scalar photon coupling (Fig. 6, upper panel)  that affects the fine-structure constant, which they extract using an optical-to-optical clock  comparison between Yb171**+ and Sr87. Quoted limit applies at the  smallest mass in their search window for this case of E-20 eV.


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SULAI 2023 looked for ultralight axion dark matter using the ``Earth as a transducer" concept  over the 0.5 to 5 Hz frequency range. They situate several magnetometers at magnetically quiet  places and search for spatially-correlated magnetic field patterns induced by axion dark matter  interacting in the effective cavity formed between the Earth's surface and the ionosphere. See  their Fig. 12 for mass-dependent limits in context. This limit extends to higher-frequencies than  their previous limit using archival geomagnetic field data collected by the SuperMAG collaboration,  see ARZA 2022


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YAO 2023 study an optical circular polarization in blazers induced by the axion-photon   mixing. The quoted limit assumes the transverse magnetic field at the jet's emission site, with   B(T) = 1 G, and this limit inversely scales with B(T). See their Fig. 3   for the limits' dependence on B(T) and electron density.


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ZHANG 2023A searched for oscillations in the fine structure constant induced by dilaton-like  dark matter by measuring the frequencies of a hyperfine-structure transition in Rb87 and  an electronic transition in Dy164, and by comparing them with that of a quartz  oscillator. They assume the local dark matter density rho_{{S}} ~= 0.4 GeV/cm**3. The  quoted limit is set at mass(S0) ~= 1E-17 eV. See their Fig. 3 for the limits over  mass(S0) = 1E-17 -- 8.3E-13 eV.


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APRILE 2022B is an update of APRILE 2020 based on a similar solar axion modeling to  DENT 2020A and GAO 2020. They exclude the XENON1T excess found in APRILE 2020.  The quoted limit holds for small g(A e e). See Fig. 6 for correlation between  G(A gamma gamma) and g(A e e).


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ARNQUIST 2022 is analogous to AVIGNONE 1998, and supersedes ANASTASSOPOULOS 2017  for mass(A0) ~> 1.2 eV.


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ARZA 2022 search for low-mass axions as dark matter using the Earth as a transducer for  axion-photon conversion. The concept works because the region between the Earth and the ionosphere  forms an insulating cavity that parametrically enhances the axion signal by the radius of the  Earth. The result is an oscillating and spatially correlated magnetic field induced via the  interaction between axion dark matter and the geomagnetic field, which they searched for using  archival magnetometer field data over 20 years compiled by the SuperMAG collaboration. Quoted limit  applies for masses 3 -- 4E-17 eV, see Fig. 1 for mass-dependent limits.


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BERNAL 2022 explored the possibility that the excess in the cosmic optical background  measured by New Horizonss Long Range Reconnaisance Imager was due to axion dark matter decaying  into monoenergetic photons. See their Fig. 2 for the axion-photon coupling to explain the excess.


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CALORE 2022 update CALORE 2020 by evaluating axion fluxes from progenitors of various  masses and performing a template-based analysis using 12 years of Fermi-LAT data in the energy  range from 50 MeV to 500 GeV. See their Fig. 10 for mass-dependent limits.


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CAPUTO 2022 study the effect of energy deposition by radiative decay of axions produced via  the Primakoff process and photon coalescence in the supernova core, and set the limits by the  radiative energy deposition < E50 erg and progenitor radius = 5E13 cm. The quoted  limit is at mass(A0) = 150 MeV. See their Fig. 2 for mass-dependent limits.


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CASTILLO 2022 update CAPUTO 2019 using the polarization measurements of the Crab Pulsar  by the QUIJOTE MFI instrument and 20 Galactic pulsars from the PPTA project. See their Table 1 for  the assumed local axion energy density rho_{{A}} for each pulsar and their Fig. 7 for the  mass-dependent limits in the range of 3E-23 eV <= mass(A0) <= E-19 eV.


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DEROCCO 2022 uses the NuSTAR data to search for monochromatic X-ray lines produced by the  decay of solar axions trapped on bound orbits. The quoted limit applies to mass(A0) ~= 9  keV. They also derive limits in the plane of g(A e e) and G(A gamma gamma).  See their Figs. 2 and 4 for mass-dependent limits.


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DESSERT 2022A look for an axion-induced linear polarization using data from multiple magnetic  white dwarf stars. See their Figs. 1 and 8 for the mass-dependent limits.


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ECKNER 2022 set limits by using sub-PeV diffuse gamma-ray data from HAWC and Tibet  ASgamma by assuming that  gamma rays produced simultaneously with high-energy neutrinos from  extragalactic sources suggested by IceCube are converted to axions in the magnetic field at the  source and reconverted to gamma rays in the Galactic magnetic field. See their Fig. 4 for  mass-dependent limits.


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FOSTER 2022 is an update of FOSTER 2020 in the list of limits on relic invisible   axions. They search for axion-photon transitions generated by neutron stars in the Galactic center  region. They use improved population models of the Galactic center neutron stars and a  Navarro-Frenk-White (NFW) model of the galactic dark matter distribution. The quoted  limit applies  to mass(A0) ~= 17 -- 25 mueV. See their Fig. 1 for  mass-dependent limits.


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KIRITA 2022 update HOMMA 2021 by increasing the laser energy and developing a  background discrimination method using the beam cross-section dependence of the background  originated from optical elements. The quoted limits applies to mass(A0) = 0.18 eV. See their Fig.  11 for mass-dependent limits.


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LANGHOFF 2022 set limits by considering the freeze-in production of axions coupled only to  photons. The quoted limit applies to mass(A0) = 2 MeV for the reheating temperature equal to 5  MeV. See their Fig. 1 for mass-dependent limits.


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LI 2022 is analogous to LI 2021B, and use the spectra of the blazar FSRQ 4C+21.35  measured by MAGIC, VERITAS, and Fermi-LAT. The quoted limit applies to mass(A0) ~= 8E-10  eV. See their Fig. 1 for mass-dependent limits.


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LI 2022C is analogous to LI 2021B, and use the  spectra of the blazars Mrk 421 and PG  1553+113 measured  by MAGIC and Fermi-LAT. The quoted limit applies to mass(A0)  ~=   1E-8  eV. See their  Fig. 4 for mass-dependent limits.


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LUCENTE 2022 developed a method to correctly incorporate the effects of axions decaying into  photons inside the core of horizontal-branch stars. They update CARENZA 2020 by evaluating  axion energy transfer in the range of axion mean free path where the diffusive energy transport and  free streaming approximations are not applicable. See their Fig. 1 for the limits.


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BASU 2021 searched for birefringence induced by axion dark matter using multiple images of  the polarized source in the strongly gravitationally lensed system CLASS B1152+199. They assume the  axion makes up all dark matter, and used the axion density in the emitting region, rho_{{A}} = 20  GeV/cm**3. Limits between 9.2E-11 -- 7.7E-8 GeV**-1 are obtained for mass(A0) =  3.6E-21 -- 4.6E-18eV. See their Fig. 2 for mass-dependent limits.


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BI 2021 look for the gamma-ray spectral distortions induced by axion-photon oscillations in  the presence of the Galactic magnetic field, 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. 3 for mass-dependent  limits.


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DOLAN 2021A study the effect of axion production on the evolution of asymptotic giant  branch  stars, and use the white-dwarf initial-final mass relation to set the limits. See their Fig.  1 for  mass-dependent limits.


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GUO 2021 is analogous to AJELLO 2016, and use the Fermi-LAT and H.E.S.S. II  measurements of PG 1553+113 and PKS 2155-304. See their Fig. 6 for mass-dependent limits.


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HOMMA 2021 look for the production of axion resonance states and their subsequent stimulated   decays by combining linearly polarized creation laser pulses and circularly polarized inducing   laser pulses. The quoted limit is at mass(A0) ~=  0.178 eV. See their Fig. 14 for   mass-dependent limits.


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LI 2021B is analogous to AJELLO 2016, and use the  spectra of the blazar Mrk 421 measured by ARGO-YBJ and Fermi-LAT. They consider ALP-photon mixing  in the magnetic fields of both the blazar jet and the Galaxy. The quoted limit applies to mass(A0)  ~= 1E-9 eV. See their Fig. 5 for mass-dependent limits.


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LLOYD 2021 is analogous to FORTIN 2018, and set limits on the product of the axion   couplings to photons and nucleons as g(A N N) G(A gamma gamma)   ~< 4.6E-19 GeV**-1 for mass(A0) ~< E-5 eV by using the quiescent soft   gamma-ray flux upper limits in five magnetars. We use g(A N N) =  G(A N)  2mass(N) to translate their limits. See their Table II and Fig. 3 for the  limits.


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REGIS 2021 look for monochromatic photons from axion decay, using the MUSE spectroscopic data  on the Leo T dwarf spheroidal galaxy. They assume that axions make up all of dark matter and use  the integrated dark matter density along the line of sight determined by observations.


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XIAO 2021 use X-ray data from Betelgeuse to look for signals from axions produced in the  stellar core that were converted to X-rays by the Galactic magnetic field. See their Fig. 1 for the  mass-dependent limit.


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ABUDINEN 2020 look for the process e+ e- --> gamma A0 (A0 --> gamma gamma) and set  upper limits of around E-3 over the mass range. The quoted limit is at mass(A0) = 0.3 GeV. See  their Fig. 5 for mass dependent limits.


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BANERJEE 2020A look for axions produced from high-energy bremsstrahlung photons  through the  Primakoff effect with the electric field of the target nuclei. They exclude G(A gamma gamma)=  2E-4 -- 5E-2 GeV**-1 for mass(A0) < 55 MeV. See their Fig. 5 for mass-dependent  limits.


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BUEHLER 2020 look for the gamma-ray transparency due to axion-photon oscillations using  high-energy photon events from 79 sources in the Second Fermi-LAT Catalog of High-Energy Sources.  The quoted limit is for the intergalactic magnetic field strength and coherence length of  B = 1 nG and s = 1 Mpc. See their Figs. 4 and 5 for mass-dependent limits and for  different magnetic-field parameters.


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CALORE 2020 use the isotropic diffuse gamma-ray background measured by the Fermi-LAT to  constrain the gamma-ray flux converted in the Galactic magnetic field from axions produced from  past core-collapse supernovae. They also derive a limit on a heavier axion with mass(A0) ~>  keV decaying into two photons of G(A gamma gamma) ~< 5E-11 GeV**-1  for mass(A0) = 5 keV.  See their Figs. 5 and 7 for the limits as well as limits in the presence of  axion-nucleon couplings.


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CARENZA 2020 extend the globular cluster bound of AYALA 2014  to heavier masses  (mass(A0) <= a few 100 keV) by taking account of the coalescence process gamma + gamma --> A0 as  well as the decay of the ALP inside the stellar core. See their Fig.4 for mass-dependent limits.


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DENT 2020A is analogous to GAO 2020. The quoted limit is from their arXiv:2006.15118v3  (v2 is their published version), using the relativistic Hartree-Fock form factor. The limit is  up to two times weaker than the published one. See Fig. 4 in their arXiv version 3 for the  correlation between G(A gamma gamma) and g(A e e) corresponding  to the excess reported in APRILE 2020.


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DEPTA 2020 correct the underestimated D abundance in MILLEA 2015, and derive  robust cosmological bounds by allowing the reheating temperature, N(eff), and  neutrino chemical potential to vary. See their Fig. 6 for mass-dependent limits.


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DESSERT 2020A use the NuSTAR data of the Quintuplet and Westerlund 1 super star clusters to  look for X-rays converted in the Galactic magnetic field from the axions produced in stellar cores.  See their Fig. 3 for the mass-dependent limits.


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ESTEBAN 2020 show that the two anomalous ANITA events can be explained by the reflected radio  pulses that are resonantly produced in the ionosphere via axion-photon conversion for mass(A0)  ~< 1E-7 eV , if an axion clump passes the Earth about once a month. See their Fig.5 for  the region consistent with this interpretation for different values of the axion density inside the  clumps.


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GAO 2020 correct the limit of APRILE 2020 by including inverse Primakoff scattering in  the XENON1T detector. The quoted limit is from their arXiv:2006.14598v4 (v3 is their published  version), taking account of the atomic form factor of Xe as pointed out in ABE 2020J. The  limit is weaker by a factor of 1.5 -- 2 than the published one. See Fig. 3 in their arXiv  version 4 for correlation between G(A gamma gamma) and g(A e e)  corresponding to the excess reported in APRILE 2020.


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KOROCHKIN 2020 assume the axion makes up all dark matter, and look for a dip in the observed  gamma-ray spectrum of the blazer 1ES 1218+304 by Fermi/LAT and VERITAS due to the extragalactic  background light produced by the axion decay. Their analysis favors nonzero axion-induced  absorption with G(A gamma gamma) = 3E-11 -- 2E-10 GeV**-1 over a range  of mass(A0) = 2 -- 18 eV. See their Fig. 1 for mass-dependent limits between 0.25 <  mass(A0) < 25 eV.


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LUCENTE 2020A study the SN 1987A energy-loss argument on the axion-like particle production.  In addition to the Primakoff process, they take account of photon coalescence as well as  gravitational trapping that become relevant at mass(A0) > 100 MeV. See their Fig. 12 for the  mass-dependent limit.


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MEYER 2020 look for prompt gamma-rays converted in the Galactic magnetic fields from  axions produced via the Primakoff process in a sample of 20 extragalactic core-collapse supernovae.  The limits assume a progenitor mass of 10 times the solar mass and certain models for the optical  emission and the galactic magnetic field. See their Figs. 2 and 6 in the erratum for mass- and  model-dependent limits.


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YAMAMOTO 2020 look for X-ray photons converted by the Earth's magnetic field from the axions  produced by the two-body decay of dark matter, and set the limits by using the Suzaku data. The  quoted limit is for the monochromatic X-ray line from the galactic dark matter with lifetime  tau = 4.32E17 sec. They also derive limits on the continuum spectrum from the  extragalactic component. See their Fig. 7 for the limits.


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ALONI 2019 used the data collected by the PRIMEX experiment to derive a limit based on a  data-driven method. See their Fig. 2 for mass-dependent limits.


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CAPUTO 2019 look for an oscillating variation of the polarization angle of the pulsar  J0437-4715, where they assume the local axion energy density rho_{{A}} = 0.3 GeV/cm**3. See  their Fig. 2 for mass-dependent limits for 5E-24 eV <= mass(A0) <= 2E-19 eV.


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FEDDERKE 2019 look for a uniform reduction of the CMB polarization at large scales, which is  induced by the oscillating axion background during CMB decoupling. The quoted limit is based on the  assumption that axions make up all of the dark matter. See their Fig. 3 for mass-dependent limits  for mass(A0) = E-22 -- E-19 eV.


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IVANOV 2019 look for the axion-induced periodic changes in the polarization angle of  parsec-scale jets in active galactic nuclei observed by the MOJAVE program, where they use the  axion energy density rho_{{A}} = 20 GeV/cm**3.  See their Fig. 6 for mass-dependent limits for  5E-23 eV <= mass(A0) <= 1.2E-21 eV.


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LIANG 2019 look for spectral irregularities in the spectrum of 10 bright H.E.S.S. sources in  the Galactic plane, assuming photon-ALP mixing in the Galactic magnetic fields. See their Fig. 2  for mass-dependent limits with different Galactic magnetic field models.


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FORTIN 2018 studied the conversion of axion-like particles produced in the core of a magnetar  to hard X-rays in the magnetosphere. See their Fig. 5 for mass-dependent limits with different  values of the magnetar core temperature.


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JAECKEL 2018 study axions produced through the Primakoff process from SN 1987A, which  subsequently decay into photon pairs. See their Fig. 1  for the mass-dependent limits in the range  of mass(A0) = 0.01 -- 100 MeV.


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YAMAJI 2018 search for axions with an x-ray LSW at Spring-8, using the Laue-case conversion  in a silicon crystal. They also obtain G(A gamma gamma) < 4.2E-3  GeV**-1 for mass(A0) < 10 eV. See their Fig. 5 for mass-dependent limits.


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ZHANG 2018 look for spectral irregularities in the spectrum of PKS 2155-304 measured by Fermi  LAT, assuming photon-ALP mixing in the intercluster and Galactic magnetic fields. See their Figs. 2  and 3 for mass-dependent limits with different values of the intercluster magnetic field parameters.


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ADE 2017 look for cosmic birefringence from axion-like particles using CMB polarization data  taken by the BICEP2 and Keck Array experiments. They set a limit G(A gamma gamma)H(I)  < 7.2E-2 at 95 %CL for mass(A0) < E-28 eV, where H(I) is  the Hubble parameter during inflation.


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ANASTASSOPOULOS 2017 looked for solar axions by the CAST axion helioscope in the vacuum  phase, and supersedes ANDRIAMONJE 2007.


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DOLAN 2017 update existing limits on G(A gamma gamma) for axion-like  particles. The limits from the proton beam dump experiments in their Fig. 2 contained an error, and  the corrected version is shown in Fig. 1 of DOLAN 2021.


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INADA 2017 search for axions with an x-ray LSW at Spring-8. See their Fig. 4 for  mass-dependent limits.


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KOHRI 2017 attributed to axion-photon oscillations the excess of cosmic infrared background  observed by the CIBER experiment. See their Fig. 5 for the region preferred by their scenario.


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MARSH 2017 is similar to WOUTERS 2013, using Chandra observations of M87. See their  Fig. 6 for mass-dependent limits.


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TIWARI 2017 use observed limits of the cosmic distance-duality relation to constrain the  photon-ALP mixing based on 3D simulations of the magnetic field configuration. The quoted value is  for the averaged magnetic field of 1nG with a coherent length of 1 Mpc. See their Fig. 5 for  mass-dependent limits.


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AJELLO 2016 look for irregularities in the energy spectrum of the NGC1275 measured by Fermi   LAT, assuming photon-ALP mixing in  the intra-cluster and Galactic magnetic fields. See their Fig.  2  for mass-dependent limits.


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DELLA-VALLE 2016 look for the birefringence induced by axion-like particles. See their Fig. 14 for mass-dependent limits.


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DELLA-VALLE 2016 look for the dichroism induced by axion-like particles. See their Fig. 14 for mass-dependent limits.


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JAECKEL 2016 use the LEP data of  and  to constrain the ALP  production via e+ e- --> Z --> A0  gamma (A0 --> gamma gamma), assuming the ALP coupling  with two hypercharge bosons. See their Fig. 4 for mass-dependent limits.


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LEEFER 2016 derived limits by using radio-frequency spectroscopy of dysprosium and atomic  clock measurements. See their Fig. 1 for mass-dependent limits as well as limits on Yukawa-type  couplings of the scalar to the electron and nucleons.


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ANASTASSOPOULOS 2015 search for solar chameleons with CAST and derived limits on the chameleon coupling to photons and matter. See their Fig. 12 for the exclusion region.


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ARIK 2015 is analogous to ARIK 2009, and search for solar axions for mass(A0) around  0.2 and 0.4 eV.  See their Figs. 1 and 3 for the mass-dependent limits.


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Based on OSQAR photon regeneration experiment.  See their Fig. 6 for mass-dependent limits on  scalar and pseudoscalar bosons.


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BRAX 2015 derived limits on conformal and disformal couplings of a scalar to photons by searching for a chaotic absorption pattern in the X-ray and UV bands of the Hydra A galaxy  cluster and a BL lac object, respectively. See their Fig. 8.


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HASEBE 2015  look for an axion via a four-wave mixing process at quasi-parallel colliding  laser beams. They also derived limits on a  scalar coupling to photons G(S gamma gamma) < 2.62E-4 GeV**-1 at mass(S0) = 0.15 eV. See their  Figs. 11 and 12 for mass-dependent limits.


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MILLEA 2015 is similar to CADAMURO 2012, including the Planck data and the latest  inferences of primordial deuterium abundance. See their Fig. 3 for mass-dependent limits.


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VANTILBURG 2015 look for harmonic variations in the dyprosium transition frequency data,  induced by coherent oscillations of the fine-structure constant due to dilaton-like dark matter,  and set the limits, G(S gamma gamma) < 6E-27 GeV**-1 at  mass(S0) =  6E-23 eV. See their Fig. 4 for mass-dependent limits between 1E-24< mass(S0)<  1E-15 eV.


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VINYOLES 2015 performed a global fit analysis based on helioseismology and solar neutrino observations. See their Fig. 9.


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AYALA 2014 derived the limit from the helium-burning lifetime of horizontal-branch stars  based on number counts in globular clusters.


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DELLA-VALLE 2014 use the new PVLAS apparatus to set a limit on vacuum magnetic birefringence induced by axion-like particles. See their Fig. 6 for the mass-dependent limits.


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EJLLI 2014 set limits on a product of primordial magnetic field and the axion mass using CMB distortion induced by resonant axion production from CMB photons. See their Fig.1 for limits applying specifically to the DFSZ and KSVZ axion models.


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PUGNAT 2014 is analogous to EHRET 2010.  See their Fig. 5 for mass-dependent limits on scalar and pseudoscalar bosons.


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REESMAN 2014 derive limits by requiring effects of axion-photon interconversion on gamma-ray  spectra from distant blazars to be no larger than errors in the  best-fit optical depth based on a  certain extragalactic background light model.  See their Fig. 5 for  mass-dependent limits.


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ABRAMOWSKI 2013A look for irregularities in the energy spectrum of the BL Lac object PKS 2155--304 measured by H.E.S.S.  The limits depend on assumed magnetic field around the source. See their Fig. 7 for mass-dependent limits.


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BETZ 2013 performed a microwave-based light shining through the wall experiment. See their Fig. 13 for mass-dependent limits.


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FRIEDLAND 2013 derived the limit by considering blue-loop suppression of the evolution of red giants with 7 -- 12 solar masses.


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MEYER 2013 attributed to axion-photon oscillations the observed excess of very high-energy gamma-rays with respect to predictions based on extragalactic background light models. See their Fig.4 for mass-dependent lower limits for various magnetic field configurations.


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WOUTERS 2013 look for irregularities in the X-ray spectrum of the Hydra cluster observed by  Chandra. See their Fig. 4 for mass-dependent limits.


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CADAMURO 2012 derived cosmological limits on G(Agammagamma) for axion-like particles. See their Fig. 1 for mass-dependent limits.


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PAYEZ 2012 derive limits from polarization measurements of quasar light (see their Fig.3). The limits depend on assumed magnetic field strength in galaxy clusters. The limits depend on assumed magnetic field and electron density in the local galaxy supercluster.


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ARIK 2011 search for solar axions using He3 buffer gas in CAST, continuing from the He4 version of ARIK 2009. See Fig.2 for the exact mass-dependent limits.


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ALPS is a photon regeneration experiment. See their Fig.4 for mass-dependent limits on scalar and pseudoscalar bosons.


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ARIK 2009 is the He4 filling version of the CAST axion helioscope in analogy to INOUE 2002 and INOUE 2008. See their Fig.7 for mass-dependent limits.


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CHOU 2009 use the GammeV apparatus in the afterglow mode to search for chameleons, (pseudo)scalar bosons with a  mass depending on the environment. For pseudoscalars they exclude at 3sigma the range 2.6E-7 GeV**-1< G(Agammagamma)< 4.2E-6 GeV**-1 for vacuum mass(A0) roughly below 6 meV for density scaling index exceeding 0.8.


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GONDOLO 2009 use the all-flavor measured solar neutrino flux to constrain solar interior temperature and thus energy losses.


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LIPSS photon regeneration experiment, assuming scalar particle S^0(). See Fig.4 for mass-dependent limits.


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CHOU 2008 perform a variable-baseline photon regeneration experiment. See their Fig.3 for mass-dependent limits. Excludes the PVLAS result of ZAVATTINI 2006.


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INOUE 2008 is an extension of INOUE 2002 to larger axion masses, using the Tokyo axion helioscope. See their Fig. 4 for mass-dependent limits.


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ZAVATTINI 2008 is an upgrade of ZAVATTINI 2006, see their Fig.8 for mass-dependent limits. They now exclude the parameter range where ZAVATTINI 2006 had seen a positive signature.


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ANDRIAMONJE 2007 looked for Primakoff conversion of solar axions in 9T superconducting magnet into X-rays.  Supersedes ZIOUTAS 2005.


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ROBILLIARD 2007 perform a photon regeneration experiment with a pulsed laser and pulsed magnetic  field. See their Fig. 4 for mass-dependent limits. Excludes the PVLAS result of ZAVATTINI 2006  with a CL exceeding 99.9%.


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ZAVATTINI 2006 propagate a laser beam in a magnetic field and observe dichroism and birefringence  effects that could be attributed to an axion-like particle. This result is now excluded by ROBILLIARD 2007, ZAVATTINI 2008, and CHOU 2008.


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MORALES 2002B looked for the coherent conversion of solar axions to photons via the Primakoff effect in Germanium detector.


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BERNABEI 2001B looked for Primakoff coherent conversion of solar axions into photons via Bragg scattering in NaI crystal in DAMA dark matter detector.


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ASTIER 2000B looked for production of axions from the interaction of high-energy photons with the horn magnetic field and their subsequent re-conversion to photons via the interaction with the NOMAD dipole magnetic field.


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MASSO 2000 studied limits on axion-proton coupling using the induced axion-photon coupling through the proton loop and CAMERON 1993 bound on the axion-photon coupling using optical rotation. They obtained the bound g(p)**2/4pi<1.7E-9 for the coupling g(p)pbargamma(5)pphi(A).


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AVIGNONE 1998 result is based on the coherent conversion of solar axions to photons via the Primakoff effect in a single crystal germanium detector.


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SEMERTZIDIS 1990 experiment is based on the proposal of MAIANI 1986. The limit is obtained by taking the noise amplitude as the upper limit.  Limits extend to mass(A0) = 4E-3 where G(A gamma gamma) < 1E-4 GeV**-1.


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AGOSTINI 2024A report a search for axion-like particle 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.


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ARNQUIST 2024 use the MAJORANA DEMONSTRATOR to search for high-mass axion-like particle dark  matter absorption by Germanium. See Fig. 5 for mass-dependent limits.


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AALBERS 2023A  look for absorption of axion dark matter. The quoted limit is for mass(A0)  ~= 1.4 keV. The local density rho_{{A}} = 0.3 GeV/cm**3 is assumed. See their Fig. 7 for  mass-dependent limits.


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ADHIKARI 2023A look for absorption and Compton-like processes of axion dark matter. The   quoted  limit is for mass(A0) ~= 37 keV. See their Fig. 4 for mass-dependent limits.


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AGNES 2023A look for absorption of axion dark matter. The quoted limit is for mass(A0)  ~= 0.25 keV. The local density rho_{{A}} = 0.3 GeV/cm**3 is assumed. See their Fig. 2 for  mass-dependent limits.


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APRILE 2023B look for an absorption signal of axions within +-500 seconds of the GW  signals, including the neutron star merger GW170817. They set a 90% CL upper limit on the  product of coincident fluence and cross section of axions to be less than E-29  cm**2/cm**2 in the recoil energy range of 5.5 -- 210 keV(ee).


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CAPOZZI 2023A search for axions produced in electromagnetic showers in proton beam dumps and  fixed target experiments. In this case, they reinterpret MiniBoone data. Quoted limit applies at 1  MeV. See Fig. 8 for mass-dependent limits.


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WADEKAR 2023 use the Leo T dwarf galaxy's interstellar medium to derive limits, requiring the  heating rate from axion dark matter absorption into hydrogen atoms and two-photon decay to be less  than the astrophysical cooling rate. See Fig. 2 for limits over mass(A0) = 1 -- 100 keV,  which loosen for lighter masses.


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APRILE 2022 extend APRILE 2019D to lower masses by removing the background of  ionization signals correlated with high-energy events.  The quoted limit applies to mass(A0) = 0.1  keV. See their Fig. 15 for mass-dependent limits.


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APRILE 2022B is an update of APRILE 2020, and set the limit, g(A e e)  ~< 9E-15 -- 3E-13. The quoted limit applies to mass(A0) = 2 keV. They exclude the  XENON1T excess found in APRILE 2020. See their Fig. 6 for mass-dependent limits.


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APRILE 2022B is an update of APRILE 2020. They exclude the XENON1T excess found in  APRILE 2020. The quoted limit holds for small G(A gamma gamma). See their  Fig. 6 for correlation between g(A e e) and G(A gamma gamma) .


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DESSERT 2022 is an update of DESSERT 2019. They used the Chandra observation of the    magnetic white dwarf RE J0317-853 to look for converted X-rays in the magnetosphere from axions    produced in the core through electron bremsstrahlung. They obtained the limit, g(A e e).G(A gamma gamma)    < 1.3E-25 GeV**-1 at 95% CL for mass(A0) ~< E-5 eV. See their Fig.   1  for mass-dependent limits.


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IKEDA 2022 look for magnons excited by dark matter axions, using data taken with a hybrid  quantum system consisting of a superconducting qubit and a spherical ferrimagnetic crystal. The  quoted limit assumes the local dark matter density rho_{{A}} = 0.45 GeV/cm**3 and the velocity  v = 220 km/sec. See their Fig. 4 for the limits.


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LANGHOFF 2022 set limits by considering the freeze-in production of axions coupled to  electrons without anomalous coupling to photons. The quoted limit applies to mass(A0) = 15 MeV for  the reheating temperature equal to 5 MeV. See their Fig. 2 for mass-dependent limits.


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WANG 2022C use the spin-amplifier based on hyperpolarized Xe129 to set limits on  the product of the axion couplings to electrons and nucleons as g(A e e)  g(A n n) < 4E2 (95 % CL) at mass(A0) = 0.1 meV. Here  g(A n n) is the dimensionless axion-neutron coupling. See their Fig. 4 for the  mass-dependent limits.


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XIAO 2022 extend XIAO 2021 in the list of photon coupling limits by including the  production of axions from Compton and bremsstrahlung processes, and set limits on the product of  the axion couplings to electrons and photons as G(A gamma gamma)  g(A e e) < 0.4 -- 2.8E-24 GeV**-1 (95 % CL) for mass(A0)  < 3.5E-11eV. See their Fig. 5 for the limits. They are comparable to those of  DESSERT 2019 and more restrictive than the CAST bounds of BARTH 2013.


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CALORE 2021 consider the production of axions from Galactic and extragalactic SNe via  nucleon-nucleon bremsstrahlung and their subsequent decay into electron-positron pairs, and exclude  the range of g(A e e) ~= E-19 -- E-11  at g(A p p) =  E-9 for mass(A0) = 3 -- 30 MeV. See their Fig. 7 for the limits.


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text:
LUCENTE 2021 study the axion production in a supernova via electron-proton bremsstrahlung and  electron-positron fusion, and exclude the range of g(A e e) ~= 2E-9 -- 5.5E-7  for masses less than 1 MeV. See their Fig. 12 for the mass-dependent limits extending up to 150  MeV. This limit was corrected in the erratum.


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AGOSTINI 2020 is analogous to AHMED 2009A. The quoted limit applies to mass(A0) = 150  keV. 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.


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AMARAL 2020 use a second-generation SuperCDMS high-voltage eV-resolution detector to set   limits on dark-matter axion absorption. The quoted limit is for mass(A0) ~= 17 eV. The  local  density rho_{{A}} = 0.3 GeV/cm**3 is assumed. See their Fig. 3 for  mass-dependent  limits.


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APRILE 2020 is an update of APRILE 2017B where they look for an absorption signal of  axion dark matter. They obtained the limit, g(A e e)  ~< 2E-14 -- 1E-12 at  90%CL for mass(A0) = 1 -- 200 keV. They also found an excess over known backgrounds,  which favors the mass mass(A0) = 2.3+-0.2 keV with a 3 sigma significance. See their  Fig. 10 for mass-dependent limits.


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text:
APRILE 2020 look for solar axions from the ABC interactions, the Primakoff conversion, and  the 14.4 keV M1 transition of Fe57, and set limits on g(A e e ),  G(A gamma gamma), g(A N N), and their products. An excess is  observed at low energies between 2 and 3 keV. See their Fig.8 for correlation between the  couplings. The quoted limit applies to the case of vanishing G(A gamma gamma) and  g(A N N).


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text:
ARALIS 2020 is analogous to AHMED 2009A. The quoted limit applies to mass(A0) = 0.3  keV. The limits at masses above 3 keV in their Fig. 9 was later found to be incorrect due to an  error in their analysis. See Fig. 2 in erratum for the corrected limits.


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CAPOZZI 2020 obtains a limit on the axion-electron coupling from the brightness of the tip of  the red-giant branch in omega Centauri. A similar limit of < 1.6E-13 is obtained  in NGC 4258.


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CRESCINI 2020 is an update of CRESCINI 2018. They assume a local axion dark matter  density, rho_{{A}} = 0.3 GeV/cm**3. See their Fig.4 for the limits.


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GHOSH 2020A study thermal production of axion via coupling to leptons in the early universe  and estimate its contribution to DeltaN(eff). The quoted limit is for  DeltaN(eff) < 0.5. See their Fig. 7 for their mass-dependent  limits.


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STRANIERO 2020 is analogous to CAPOZZI 2020, with 22 galactic globular clusters used to  derive the limit.


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WANG 2020A is an update of LIU 2017A. They assume a local axion dark matter density,  rho_{{A}} = 0.3 GeV/cm**3. See their Fig. 10 for limits between 0.185 < mass(A0) <  10 keV.


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text:
APRILE 2019D is analogous to APRILE 2017B, but they use only ionization signals. The  quoted limit applies to mass(A0) = 0.7 keV. See their Fig. 5(e) for mass-dependent limits.


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DESSERT 2019 used the Suzaku observations of a magnetic white dwarf (RE J0317-853) to look  for X-ray signatures converted from axions in the surrounding magnetic fields. They obtained the  limit, g(A e e).G(A gamma gamma) < 1.6E-24  GeV**-1 at 95%CL for mass(A0) ~< E-5 eV. See their Fig. 2 for mass-dependent  limits.


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TERRANO 2019 look for the axion-induced oscillating magnetic field acting on the electron  spin, using data taken with a rotating torsion pendulum containing polarized electrons. The quoted  limit applies to mass(A0) = E-23 -- E-18 eV  and assumes a local axion dark matter density,  rho_{{A}} = 0.45 GeV/cm**3. See their Fig. 5 for mass-dependent limits.


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ABE 2018F is an update of ABE 2014F. The quoted limit applies to mass(A0) = 60 keV.  See their Fig. 5 for mass-dependent limits.


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ARMENGAUD 2018 is analogous to AHMED 2009A. See the left panel of Fig. 5 for  mass-dependent limits.


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CRESCINI 2018 look for collective excitations of the electron spins caused by dark matter  axions. The quoted limit assumes the local dark matter density, rho_{{A}} = 0.45 GeV/cm**3.


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FICEK 2018 use the measurements of the hyperfine structure of antiprotonic helium to  constrain a dipole-dipole potential between electron and antiproton. See their Fig. 3 for limits on  various spin- and velocity-dependent potentials.


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ABGRALL 2017 is analogous to AHMED 2009A using the MAJORANA DEMONSTRATOR. See their  Fig. 2 for limits between 6 keV < mass(A0) < 97 keV.


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APRILE 2017B is analogous to AHMED 2009A. They found a bug in their code and needed to  correct the limits in Fig. 7 of APRILE 2014B. See their Fig. 1 for the corrected limits  between 1 keV < mass(A0) < 40 keV.


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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.


pdgid: S029IAN
text:
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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text:
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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text:
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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text:
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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text:
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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text:
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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text:
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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text:
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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text:
BHUSAL 2021 looked for 5.5 MeV solar axions produced by p d --> He3A0  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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text:
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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text:
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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text:
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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text:
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).


pdgid: S029IAN
text:
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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text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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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text:
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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text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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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text:
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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text:
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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text:
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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text:
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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text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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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text:
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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text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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.


pdgid: S029IAN
text:
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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text:
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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text:
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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text:
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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text:
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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text:
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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text:
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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text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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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text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
IGNATOVICH 2009 use data on depolarization of ultracold neutrons in material traps. They show lambda-dependent limits in their Fig. 1.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
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.


pdgid: S029IAT
text:
NI 1999 searched for a T-violating medium-range force acting on paramagnetic Tb F(3) salt.  See their Fig.1 for the result.


pdgid: S029IAT
text:
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 (1cm/lambda(A)), where lambda(A)=hbar/mass(A)c.


pdgid: S029IAT
text:
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:
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  >3.7yr. 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:
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 2024is a combination of their new result of the 2021 data (<7.5) with the  previous BALDINI 2016 results. 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 0.1T 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: S004ETA
text:
Global fit to all measured parameters.  The fit correlation coefficients are given in BURKARD 1985B.


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.


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


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:
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)| = cottheta(W)|d(tau)**W| using effective Lagrangian methods, and use a conference result |d(tau)**W| <5.8E-18ecm 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:
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 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. (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:
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 LEP1 data on taubranching 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: 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:
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: 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 etal. (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 etal. (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.


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 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:
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 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 ``nubarMass 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 ``nubarMass 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 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:
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 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+-2.2eV**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: S066MNM
text:
ASSAMAGAN 1996 measurement of p_{{mu}} from pi+ --> mu+ nu at rest combined with JECKELMANN 1994 SolutionB pion mass yields mass**2(nu) = -0.016+-0.023 with corresponding Bayesian limit listed above. If SolutionA 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, ~1s.


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 taumass 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 20MeV 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 300s.  For Dirac neutrinos limits change to <0.3 or >33.


pdgid: S066MNT
text:
KAWASAKI 1994 excluded region is for Majorana neutrino with lifetime >1000s. 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 >100s. 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:
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:
ABBOTT 2021A combines Dark Energy Survey (DES) year 3 results with Planck CMB lensing  measurements.


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  <0.24eV. 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 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 typeIa, 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 0.9eV assuming 3nearly 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:
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 (<5keV) 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 (<1keV) 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 tonu_{{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 nuflux from p p, now established from GALLEX and SAGE to be >0.5 of expectation.


pdgid: S066TMR
text:
To obtain the limit 6E7s 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 ~<0.14eV.


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-3eV**2 to obtain tau(13)/m(1)**3 > 1E23s/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**7s/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 1.5E3seV**-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-associatednu 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 1eV. Curve shows tau(nu)/B(gamma)>0.15E21s at 0.05eV, >1.2E21s at 0.17eV, >3E21s at 1eV, where B(gamma) is the branching ratio to photons.


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


pdgid: S066TMR
text:
Limit on the radiative decay based on nonobservation of gamma's in coincidence with nu's from SN1987A.


pdgid: S066TMR
text:
DODELSON 1992 range is for wrong-helicity keV mass Dirac nu's from the core of neutron star in SN1987A 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 > 3E18s 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 SN1987A 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**23s 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:
CARENZA 2024A derive the limit from the production of right-handed neutrinos in the early  universe.


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 (<5keV) 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 (<1keV) 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**-9G/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:
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:
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:
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 1sigma errors.


pdgid: S007NE
text:
JANOT 2020 applies a correction to LEP-SLC 2006 using an updated Bhabha cross section  calculation. This result also includes a correction to account for correlated luminosity bias as  presented in VOUTSINAS 2020.


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:
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:
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:
ABE 2023 use the combined data set of the KamLAND-Zen 400 and 800 experiments, utilizing 745  kg of isotopically enriched xenon (90.9% Xe136), dissolved in liquid scintillator  and an exposure of 970 kg.yr of Xe136, to derive this limit on 0nubeta beta  decay. A half-life sensitivity of 1.5E26 yr is reported.


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:
ADAMS 2020A use the CUORE detector to search for the 0nu beta beta decay of  Te130. The exposure was 372.5 kg.yr of TeO(2) corresponding to 103.6  kg.yr of Te130. The exclusion sensitivity is 1.7E25yr. Supersedes  ALDUINO 2018.


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:
ALENKOV 2019 report the 0nu beta beta decay half-life limit  based on the 52.1  kg.d exposure of Mo100, of a a cryogenic dual heat and light detector in the  Yangyang underground laboratory. The median sensitivity is 1.1E23 years.


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.


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:
ADAMS 2021 use 102.7 kg yr of Te130 exposure, collected by the CUORE bolometric  detector at LNGS, to perform a measurement of the 2nu beta beta decay of Te130.  The dataset is more than 10-times that collected by the CUORE-0 experiment. The result has been  revised in ADAMS 2023A. Supersedes ALDUINO 2017.


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 2023 utilize 745 kg of Xe136 isotope exposure from the combined data set of  the KamLAND-Zen 400 and 800 to derive a limit on <mass(beta beta)>. The range  reflects the author's assessment of the variability of the theoretically calculated 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 2.6E23y 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 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 ~180km baseline to various Japanese nuclear power reactors.


pdgid: S067RER
text:
BOEHM 2001 search for neutrino oscillations at 0.75 and 0.89km distance from the Palo Verde reactors.


pdgid: S067RER
text:
APOLLONIO 1999, APOLLONIO 1998 search for neutrino oscillations at 1.1km 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 18m and 24m 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 ktonyr 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 ktonyr 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 4GeV.  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 4GeV.  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 1GeV. 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 nus and nubars, 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:
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 5MeV.  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 KamiokandeII and III from January 1987 through February 1995, covering the entire solar cycle22, with threshold E(e)>9.3MeV (first 449 days), >7.5MeV (middle 794 days), and >7.0MeV (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 5MeV.  The data correspond to 306.4 live days with SNO between November 2, 1999 and May 28, 2001, and updates AHMAD 2001 results.


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.


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: 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.


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:
The measurement of the B8 flux mostly comes from the NC signal, however, CC contribution is included in the fit.


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 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.


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**-2s**-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-46cm**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:
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:
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: 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 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: S067DM3
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: S067DM3
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: 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:
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: 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:
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:
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 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:
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:
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:
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:
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:
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:
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 data are separated into pure samples of nus and nubars, and separate oscillation parameters for nus 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.


