#### Limit on Invisible ${{\mathit A}^{0}}$ (Axion) Electron Coupling

The limit is for $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$ $\phi _{A}{{\overline{\mathit e}}}$ ($\mathit i$ $\gamma _{5}){{\mathit e}}$ , or equivalently, the dipole-dipole potential $−{\mathit g{}^{2}_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }\over 16{{\mathit \pi}} {{\mathit m}^{2}}_{{{\mathit e}}}}$ (($\mathbf {\sigma }_{1}\cdot{}\mathbf {\sigma }_{2}$) $-3(\mathbf {\sigma }_{1}\cdot{}\mathbf {\mathit n}$) ($\mathbf {\sigma }_{2}\cdot{}\mathbf {\mathit n}))/\mathit r{}^{3}$ where $\mathbf {\mathit n}=\mathbf {\mathit r}/\mathit r$ and the sign of the potential was corrected based on DAIDO 2017 .

VALUE CL% DOCUMENT ID TECN  COMMENT
• • We do not use the following data for averages, fits, limits, etc. • •
1
 2021
ASTR Core-collapse SNe
$<2.5 \times 10^{-10}$ 2
 2021
ASTR SN 1987A
$<3 \times 10^{-12}$ 90 3
 2020
HPGE ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.06 - 1$ MeV
$<1 \times 10^{-9}$ 90 4
 2020
SCDM ${\mathit m}_{{{\mathit A}^{0}}}$ = $1.2 - 50$ eV
$<2 \times 10^{-14}$ 90 5
 2020
XE1T ${\mathit m}_{{{\mathit A}^{0}}}$ = 1 keV
$2.6 - 3.7 \times 10^{-12}$ 90 6
 2020
XE1T Solar axions
$<6 \times 10^{-13}$ 90 7
 2020
SCDM ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.04 - 500$ keV
$<1.3 \times 10^{-13}$ 95 8
 2020
ASTR Tip of the Red Giant Branch
$<1.7 \times 10^{-11}$ 95 9
 2020
QUAX ${\mathit m}_{{{\mathit A}^{0}}}$ = $42.4 - 43.1$ $\mu$eV
$<1.8 \times 10^{-9}$ 10
 2020 A
COSM ${\mathit m}_{{{\mathit A}^{0}}}{ {}\lesssim{} }$ 0.5 MeV
$<1.48 \times 10^{-13}$ 95 11
 2020
ASTR Tip of the Red Giant Branch
$<2.48 \times 10^{-11}$ 90 12
 2020 A
CDEX Solar axions
$<4 \times 10^{-13}$ 90 13
 2020 A
CDEX ${\mathit m}_{{{\mathit A}^{0}}}$ = 1.5 keV
$<1.7 \times 10^{-11}$ 90 14
 2019 B
C100 Solar axions
$<2.3 \times 10^{-14}$ 90 15
 2019 D
XE1T ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.186 - 1$ keV
16
 2019
ASTR Magnetic white dwarf
$<2.6 \times 10^{-10}$ 95 17
 2019
Torsion pendulum
$<1.5 \times 10^{-13}$ 90 18
 2018 F
XMAS ${\mathit m}_{{{\mathit A}^{0}}}$ = $40 - 120$ keV
$<1.1 \times 10^{-11}$ 90 19
 2018
EDE3 Solar axions
$<4 \times 10^{-13}$ 90 20
 2018
EDE3 ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.8 - 500$ keV
$<4.9 \times 10^{-10}$ 95 21
 2018
QUAX ${\mathit m}_{{{\mathit A}^{0}}}$ = 58 $\mu$eV
22
 2018
THEO ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 10 keV
$<4.5 \times 10^{-13}$ 90 23
 2017
HPGE ${\mathit m}_{{{\mathit A}^{0}}}$ = 11.8 keV
$<3.5 \times 10^{-12}$ 90 24
 2017 B
LUX Solar axions
$<4.2 \times 10^{-13}$ 90 25
 2017 B
LUX ${\mathit m}_{{{\mathit A}^{0}}}$ = $1 - 16$ keV
$<2.3 \times 10^{-13}$ 90 26
 2017 B
X100 ${\mathit m}_{{{\mathit A}^{0}}}$ = 6 keV
$<4 \times 10^{-4}$ 90 27
 2017
THEO ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 1 keV
$<4.35 \times 10^{-12}$ 90 28
 2017 A
PNDX Solar axions
$<4.3 \times 10^{-14}$ 90 29
 2017 A
PNDX ${\mathit m}_{{{\mathit A}^{0}}}$ = 2 keV
$<5 \times 10^{-13}$ 90 30
 2017 A
CDEX ${\mathit m}_{{{\mathit A}^{0}}}$ = 13 keV
$<2.5 \times 10^{-11}$ 90 31
 2017 A
CDEX Solar axions
$<0.15$ 95 32
 2017
${\mathit m}_{{{\mathit A}^{0}}}$ = 300 eV
$<3.3 \times 10^{-13}$ 68 33
 2016
ASTR White dwarf cooling
$<7 \times 10^{-13}$ 34
 2016
ASTR White dwarf cooling
$<1.39 \times 10^{-11}$ 90 35
 2016
KIMS Solar axions
$<7.4 \times 10^{-9}$ 95 36
 2015
${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 30 $\mu$eV
$<8 \times 10^{-13}$ 90 37
 2014 F
XMAS ${\mathit m}_{{{\mathit A}^{0}}}$ = 60 keV
$<7.7 \times 10^{-12}$ 90 38
 2014 B
X100 Solar axions
39
 2014 B
X100 ${\mathit m}_{{{\mathit A}^{0}}}$ = $5 - 7$ keV
$< 0.96 - 8.2 \times 10^{-8}$ 90 40
 2014
CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.1 - 1$ MeV
$<2.8 \times 10^{-13}$ 99 41
 2014
ASTR White dwarf cooling
$<5.4 \times 10^{-11}$ 90 42
 2013 D
XMAS Solar axions
$<1.07 \times 10^{-12}$ 90 43
 2013
EDEL ${\mathit m}_{{{\mathit A}^{0}}}$ = 12.5 keV
$<2.59 \times 10^{-11}$ 90 44
 2013
EDEL Solar axions
45
 2013
CAST Solar axions
$< 1.4 - 9.7 \times 10^{-7}$ 90 46
 2013
CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.1 - 1$ MeV
$<1.5 \times 10^{-8}$ 68 47
 2013
${\mathit m}_{{{\mathit A}^{0}}}{}\leq{}$ 0.1 $\mu$eV
$<4.3 \times 10^{-13}$ 95 48
 2013 A
ASTR Low-mass red giants
$<7 \times 10^{-13}$ 95 49
 2012
ASTR White dwarf cooling
$<2.2 \times 10^{-10}$ 90 50
 2012
CNTR Solar axions
$<0.02 - 1 \times 10^{-10}$ 90 51
 2011
CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.3 - 8$ keV
$<1.4 \times 10^{-12}$ 90 52
 2009 A
CDMS ${\mathit m}_{{{\mathit A}^{0}}}$ = 2.5 keV
$<4 \times 10^{-9}$ 53
 2009
ASTR Earth cooling
$<2.7 \times 10^{-8}$ 66 54
 1994
Induced magnetism
54
 1993
Induced magnetism
$<3.6 \times 10^{-7}$ 66 55
 1992
Torsion pendulum
$<2.9 \times 10^{-8}$ 95 54
 1991
Induced magnetism
$<1.9 \times 10^{-6}$ 66 56
 1991
NMR
$<7 \times 10^{-7}$ 66 55
 1990
Torsion pendulum
$<6.6 \times 10^{-8}$ 95 54
 1988
Induced magnetism
 1 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 $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$ $\simeq{}$ $10^{-19} - 10^{-11}$ at $\mathit g_{ {{\mathit A}} {{\mathit p}} {{\mathit p}} }$ = $10^{-9}$ for ${\mathit m}_{{{\mathit A}^{0}}}$ = $3 - 30$ MeV. See their Fig. 7 for the limits.
 2 LUCENTE 2021 study the axion production in a supernova via electron-proton bremsstrahlung and electron-positron fusion, and exclude the range of $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$ $\simeq{}$ $10^{-10} - 10^{-8}$ for ${\mathit m}_{{{\mathit A}^{0}}}$ = $1 - 160$ MeV. The quoted limit is at ${\mathit m}_{{{\mathit A}^{0}}}$ = 120 MeV. See their Fig. 12 for the mass-dependent limits.
 3 AGOSTINI 2020 is analogous to AHMED 2009A. The quoted limit applies to ${\mathit m}_{{{\mathit A}^{0}}}$ = 150 keV. See their Fig.3 for mass-dependent limits.
 4 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 ${\mathit m}_{{{\mathit A}^{0}}}$ $\simeq{}$ 17 eV. The local density $\rho _{{{\mathit \gamma}^{\,'}} }$ = 0.3 GeV/cm${}^{3}$ is assumed. See their Fig. 3 for mass-dependent limits.
 5 APRILE 2020 is an update of APRILE 2017B where they look for an absorption signal of axion dark matter. They obtained the limit, $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$ ${ {}\lesssim{} }$ $2 \times 10^{-14} - 1 \times 10^{-12}$ at 90$\%$CL for ${\mathit m}_{{{\mathit A}^{0}}}$ = $1 - 200$ keV. They also found an excess over known backgrounds, which favors the mass ${\mathit m}_{{{\mathit A}^{0}}}$ = $2.3$ $\pm0.2$ keV with a 3 $\sigma$ significance. See their Fig. 10 for mass-dependent limits.
 6 APRILE 2020 look for solar axions from the ABC interactions, the Primakoff conversion, and the 14.4 keV M1 transition of ${}^{57}\mathrm {Fe}$, and set limits on $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$, $\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }$, $\mathit g_{ {{\mathit A}} {{\mathit N}} {{\mathit N}} }$, 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 $\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }$ and $\mathit g_{ {{\mathit A}} {{\mathit N}} {{\mathit N}} }$.
 7 ARALIS 2020 is analogous to AHMED 2009A. The quoted limit applies to ${\mathit m}_{{{\mathit A}^{0}}}$ = 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 ARALIS 2021 for the corrected limits.
 8 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 $<$ $1.6 \times 10^{-13}$ is obtained in NGC 4258.
 9 CRESCINI 2020 is an update of CRESCINI 2018 . They assume a local axion dark matter density, ${{\mathit \rho}_{{A}}}$ = 0.3 GeV/cm${}^{3}$. See their Fig.4 for the limits.
 10 GHOSH 2020A study thermal production of axion via coupling to leptons in the early universe and estimate its contribution to $\Delta \mathit N_{{\mathrm {eff}}}$. The quoted limit is for $\Delta \mathit N_{{\mathrm {eff}}}$ $<$ 0.5. See their Fig. 7 for their mass-dependent limits.
 11 STRANIERO 2020 is analogous to CAPOZZI 2020 , with 22 galactic globular clusters used to derive the limit.
 12 WANG 2020A is an update of LIU 2017A. See their Fig. 9.
 13 WANG 2020A is an update of LIU 2017A. They assume a local axion dark matter density, ${{\mathit \rho}_{{A}}}$ = 0.3 GeV/cm${}^{3}$. See their Fig. 10 for limits between 0.185 $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 10 keV.
 14 ADHIKARI 2019B is analogous to LIU 2017A.
 15 APRILE 2019D is analogous to APRILE 2017B, but they use only ionization signals. The quoted limit applies to ${\mathit m}_{{{\mathit A}^{0}}}$ = 0.7 keV. See their Fig. 5(e) for mass-dependent limits.
 16 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, $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }\cdot{}\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }$ $<$ $1.6 \times 10^{-24}$ GeV${}^{-1}$ at 95$\%$CL for ${\mathit m}_{{{\mathit A}^{0}}}{ {}\lesssim{} }$ $10^{-5}$ eV. See their Fig. 2 for mass-dependent limits.
 17 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 ${\mathit m}_{{{\mathit A}^{0}}}$ = $10^{-23} - 10^{-18}$ eV and assumes a local axion dark matter density, ${{\mathit \rho}_{{A}}}$ = 0.45 GeV/cm${}^{3}$. See their Fig. 5 for mass-dependent limits.
 18 ABE 2018F is an update of ABE 2014F. The quoted limit applies to ${\mathit m}_{{{\mathit A}^{0}}}$ = 60 keV. See their Fig. 5 for mass-dependent limits.
 19 ARMENGAUD 2018 is analogous to LIU 2017A.
 20 ARMENGAUD 2018 is analogous to AHMED 2009A. See the left panel of Fig. 5 for mass-dependent limits.
 21 CRESCINI 2018 look for collective excitations of the electron spins caused by dark matter axions. The quoted limit assumes the local dark matter density, ${{\mathit \rho}_{{A}}}$ = 0.45 GeV/cm${}^{3}$.
 22 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.
 23 ABGRALL 2017 is analogous to AHMED 2009A using the MAJORANA DEMONSTRATOR. See their Fig. 2 for limits between 6 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 97 keV.
 24 AKERIB 2017B is analogous to LIU 2017A.
 25 AKERIB 2017B is analogous to AHMED 2009A. See their Fig. 7 for mass-dependent limits.
 26 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 $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 40 keV.
 27 FICEK 2017 look for spin-dependent interactions between electrons by comparing precision spectroscopic measurements in ${}^{4}\mathrm {He}$ with theoretical calculations. See their Fig. 1 for limits up to ${\mathit m}_{{{\mathit A}^{0}}}$ = 10 keV.
 28 FU 2017A is analogous to LIU 2017A. See their Fig. 3 for mass-dependent limits.
 29 FU 2017A is analogous to AHMED 2009A. See their Fig. 4 for mass-dependent limits.
 30 LIU 2017A is analogous to AHMED 2009A. See their Fig. 9 for limits between 0.25 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 20 keV.
 31 LIU 2017A look for solar axions produced from Compton, bremsstrahlung, atomic-recombination and deexcitation channels, and set a limit for ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 1 keV.
 32 LUO 2017 use a recent measurement of the dipole-dipole interaction between two iron atoms at the nanometer scale and set a limit for ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 1 keV. See their Fig. 3 for mass-dependent limits.
 33 BATTICH 2016 is analogous to CORSICO 2016 and used the pulsating DB white dwarf PG 1351+489.
 34 CORSICO 2016 studied the cooling rate of the pulsating DA white dwarf L19-2 based on an asteroseismic model.
 35 YOON 2016 look for solar axions with the axio-electric effect in ${}^{}\mathrm {CsI}({}^{}\mathrm {Tl}$) crystals and set a limit for ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 1 keV.
 36 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 ${\mathit m}_{{{\mathit A}^{0}}}$ = 500 $\mu$eV.
 37 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 ${\mathit m}_{{{\mathit A}^{0}}}$ = $40 - 120$ keV.
 38 APRILE 2014B look for solar axions using the XENON100 detector.
 39 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.
 40 DERBIN 2014 is an update of DERBIN 2013 with a BGO scintillating bolometer. See their Fig. 3 for mass-dependent limits.
 41 MILLER-BERTOLAMI 2014 studied the impact of axion emission on white dwarf cooling in a self-consistent way.
 42 ABE 2013D is analogous to DERBIN 2012 , using the XMASS detector.
 43 ARMENGAUD 2013 is similar to AALSETH 2011 . See their Fig. 10 for limits between 3 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}<$ 100 keV.
 44 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.
 45 BARTH 2013 search for solar axions produced by axion-electron coupling, and obtained the limit, $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }\cdot{}\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }<$ $8.1 \times 10^{-23}$ GeV${}^{-1}$ at 95$\%$CL.
 46 DERBIN 2013 looked for 5.5 MeV solar axions produced in ${{\mathit p}}$ ${{\mathit d}}$ $\rightarrow$ ${}^{3}\mathrm {He}{{\mathit A}^{0}}$ in a BGO detector through the axioelectric effect. See their Fig. 4 for mass-dependent limits.
 47 HECKEL 2013 studied the influence of 2 or 4 stationary sources each containing $6.0 \times 10^{24}$ polarized electrons, on a rotating torsion pendulum containing $9.8 \times 10^{24}$ polarized electrons. See their Fig. 4 for mass-dependent limits.
 48 VIAUX 2013A constrain axion emission using the observed brightness of the tip of the red-giant branch in the globular cluster M5.
 49 CORSICO 2012 attributed the excessive cooling rate of the pulsating white dwarf R548 to emission of axions with $\mathit g_{{{\mathit A}} {{\mathit e}} {{\mathit e}} }$ $\simeq{}$ $4.8 \times 10^{-13}$.
 50 DERBIN 2012 look for solar axions with the axio-electric effect in a ${}^{}\mathrm {Si}({}^{}\mathrm {Li}$) detector. The solar production is based on Compton and bremsstrahlung processes.
 51 AALSETH 2011 is analogous to AHMED 2009A. See their Fig.$~$4 for mass-dependent limits.
 52 AHMED 2009A assume keV-mass pseudoscalars are the local dark matter and constrain the axio-electric effect in the CDMS detector. See their Fig.$~$5 for mass-dependent limits.
 53 DAVOUDIASL 2009 use geophysical constraints on Earth cooling by axion emission.
 54 These experiments measured induced magnetization of a bulk material by the spin-dependent potential generated from other bulk material with aligned electron spins, where the magnetic field is shielded with superconductor. The sign of the limit set by CHUI 1993 is opposite to that of the axion-mediated dipole-dipole potential.
 55 These experiments used a torsion pendulum to measure the potential between two bulk matter objects where the spins are polarized but without a net magnetic field in either of them. The limits reflect the corrected sign of the dipole-dipole potential.
 56 WINELAND 1991 looked for an effect of bulk matter with aligned electron spins on atomic hyperfine splitting using nuclear magnetic resonance.
References:
 CALORE 2021
PR D104 043016 Supernova bounds on axionlike particles coupled with nucleons and electrons
 LUCENTE 2021
PR D104 103007
 AGOSTINI 2020
PRL 125 011801 The first search for bosonic super-WIMPs with masses up to 1 MeV/c$^2$ with GERDA
 AMARAL 2020
PR D102 091101 Constraints on low-mass, relic dark matter candidates from a surface-operated SuperCDMS single-charge sensitive detector
 APRILE 2020
PR D102 072004 Excess electronic recoil events in XENON1T
 ARALIS 2020
PR D101 052008 Constraints on dark photons and axionlike particles from the SuperCDMS Soudan experiment
 Also
PR D103 039901 (errat.) Constraints on dark photons and axionlike particles from the SuperCDMS Soudan experiment
 CAPOZZI 2020
PR D102 083007 Axion and neutrino bounds improved with new calibrations of the tip of the red-giant branch using geometric distance determinations
 CRESCINI 2020
PRL 124 171801 Axion search with a quantum-limited ferromagnetic haloscope
 GHOSH 2020A
JCAP 2010 060 Constraints on Axion-Lepton coupling from Big Bang Nucleosynthesis
 STRANIERO 2020
AA 644 A166 The RGB tip of galactic globular clusters and the revision of the axion-electron coupling bound
 WANG 2020A
PR D101 052003 Improved limits on solar axions and bosonic dark matter from the CDEX-1B experiment using the profile likelihood ratio method
ASP 114 101 A search for solar axion induced signals with COSINE-100
 APRILE 2019D
PRL 123 251801 Light Dark Matter Search with Ionization Signals in XENON1T
 DESSERT 2019
PRL 123 061104 X-ray signatures of axion conversion in magnetic white dwarf stars
 TERRANO 2019
PRL 122 231301 Constraints on axionlike dark matter with masses down to $10^{-23}$ eV/c$^2$
 ABE 2018F
PL B787 153 Search for dark matter in the form of hidden photons and axion-like particles in the XMASS detector
 ARMENGAUD 2018
PR D98 082004 Searches for electron interactions induced by new physics in the EDELWEISS-III Germanium bolometers
 CRESCINI 2018
EPJ C78 703 Operation of a ferromagnetic axion haloscope at $m_a=58\,\mu$eV
 FICEK 2018
PRL 120 183002 Constraints on exotic spin-dependent interactions between matter and antimatter from antiprotonic helium spectroscopy
 ABGRALL 2017
PRL 118 161801 New limits on Bosonic Dark Matter, Solar Axions, Pauli Exclusion Principle Violation, and Electron Decay from the Majorana Demonstrator
 AKERIB 2017B
PRL 118 261301 First Searches for Axions and Axionlike Particles with the LUX Experiment
 APRILE 2017B
PR D95 029904 Erratum to APRILE 2014B: First Axion Results from the XENON100 Experiment
 FICEK 2017
PR A95 032505 Constraints on Exotic Spin-Dependent Interactions between Electrons from Helium Fine-Structure Spectroscopy
 FU 2017A
PRL 119 181806 Limits on Axion Couplings from the First 80 Days of Data of the PandaX-II Experiment
 LIU 2017A
PR D95 052006 Constraints on Axion Couplings from the CDEX-1 Experiment at the China Jinping Underground Laboratory
 LUO 2017
PR D96 055028 Constraints on Spin-Dependent Exotic Interactions between Electrons at the Nanometer Scale
 BATTICH 2016
JCAP 1608 062 First Axion Bounds from a Pulsating Helium-Rich White Dwarf Star
 CORSICO 2016
JCAP 1607 036 An Asteroseismic Constraint on the Mass of the Axion from the Period Drift of the Pulsating DA White Dwarf Star L19-2
 YOON 2016
JHEP 1606 011 Search for Solar Axions with CsI(Tl) Crystal Detectors
 TERRANO 2015
PRL 115 201801 Short-Range Spin-Dependent Interactions of Electrons: a Probe for Exotic Pseudo-Goldstone Bosons
 ABE 2014F
PRL 113 121301 Search for Bosonic Superweakly Interacting Massive Dark Matter Particles with the XMASS-I Detector
 APRILE 2014B
PR D90 062009 First Axion Results from the XENON100 Experiment
 DERBIN 2014
EPJ C74 3035 Search for Axioelectric Effect of Solar Axions using BGO Scintillating Bolometer
 MILLER-BERTOLAMI 2014
JCAP 1410 069 Revisiting the Axion Bounds from the Galactic White Dwarf Luminosity Function
 ABE 2013D
PL B724 46 Search for Solar Axions in XMASS, a Large Liquid-Xenon Detector
 ARMENGAUD 2013
JCAP 1311 067 Axion Searches with the EDELWEISS-II Experiment
 BARTH 2013
JCAP 1305 010 CAST Constraints on the Axion-Electron Coupling
 DERBIN 2013
EPJ C73 2490 Search for Axioelectric Effect of 5.5 MeV Solar Axions using BGO Detectors
 HECKEL 2013
PRL 111 151802 Limits on Exotic Long-Range Spin-Spin Interactions of Electrons
 VIAUX 2013A
PRL 111 231301 Neutrino and Axion Bounds from the Globular Cluster M5 (NGC 5904)
 CORSICO 2012
JCAP 1212 010 An Independent Limit on the Axion Mass from the Variable White Dwarf Star R548
 DERBIN 2012
JETPL 95 339 Constraints on the Axion-Electron Coupling Constant for Solar Axions Appearing Owing to Bremsstrahlung and the Compton Process
 AALSETH 2011
PRL 106 131301 Results from a Search for Light-Mass Dark Matter with a $\mathit p$-Type Point Contact Germanium Detector
 AHMED 2009A
PRL 103 141802 Search for Axions with the CDMS Experiment
 DAVOUDIASL 2009
PR D79 095024 Thermal Production of Axions in the Earth
 NI 1994
Physica B194 153 Search for Anomalous Spin-Spin Interactions between Electrons using a DC SQUID
 CHUI 1993
PRL 71 3247 Experimental Search for Anomalous Spin-Spin Interaction between Electrons
 PAN 1992
MPL A7 1287 Experimental Search for Anomalous Spin-Spin Interactions
 BOBRAKOV 1991
JETPL 53 294 An Experimental Limit on the Existence of the Electron Quasimagnetic (Arion) Interaction
 WINELAND 1991
PRL 67 1735 Search for Anomalous Spin Dependent Forces Using Stored Ion Spectroscopy
 RITTER 1990
PR D42 977 Experimental Test of Equivalence Principle with Polarized Masses
 VOROBYOV 1988
PL B208 146 New Limit on the Arion Interaction Constant