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. • • $<4 \times 10^{-12}$ 90 1 APRILE 2022 XE1T ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.01 - 0.4$ keV $<9 \times 10^{-15}$ 90 2 APRILE 2022 B XENT ${\mathit m}_{{{\mathit A}^{0}}}$ = $1 - 39$, $44 - 140$ keV $<2 \times 10^{-12}$ 90 3 APRILE 2022 B XENT Solar axions 4 DESSERT 2022 ASTR Magnetic white dwarf $<2.6 \times 10^{-6}$ 95 5 IKEDA 2022 ${\mathit m}_{{{\mathit A}^{0}}}=33.117 - 33.130$ $\mu $eV $<2.5 \times 10^{-18}$ 6 LANGHOFF 2022 COSM ${\mathit m}_{{{\mathit A}^{0}}}$ = $20 - 3 \times 10^{4}$ keV 7 WANG 2022 C ${\mathit m}_{{{\mathit A}^{0}}}{}\leq{}$ 0.47 meV 8 XIAO 2022 ASTR Betelgeuse 9 CALORE 2021 ASTR Core-collapse SNe $<2.5 \times 10^{-10}$ 10 LUCENTE 2021 ASTR SN 1987A $<5.1 \times 10^{-12}$ 90 11 AGOSTINI 2020 HPGE ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.06 - 1$ MeV $<1 \times 10^{-9}$ 90 12 AMARAL 2020 SCDM ${\mathit m}_{{{\mathit A}^{0}}}$ = $1.2 - 50$ eV $<2 \times 10^{-14}$ 90 13 APRILE 2020 XE1T ${\mathit m}_{{{\mathit A}^{0}}}$ = 1 keV $2.6 - 3.7 \times 10^{-12}$ 90 14 APRILE 2020 XE1T Solar axions $<6 \times 10^{-13}$ 90 15 ARALIS 2020 SCDM ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.04 - 500$ keV $<1.3 \times 10^{-13}$ 95 16 CAPOZZI 2020 ASTR Tip of the Red Giant Branch $<1.7 \times 10^{-11}$ 95 17 CRESCINI 2020 QUAX ${\mathit m}_{{{\mathit A}^{0}}}$ = $42.4 - 43.1$ $\mu $eV $<1.8 \times 10^{-9}$ 18 GHOSH 2020 A COSM ${\mathit m}_{{{\mathit A}^{0}}}{ {}\lesssim{} }$ 0.5 MeV $<1.48 \times 10^{-13}$ 95 19 STRANIERO 2020 ASTR Tip of the Red Giant Branch $<2.48 \times 10^{-11}$ 90 20 WANG 2020 A CDEX Solar axions $<4 \times 10^{-13}$ 90 21 WANG 2020 A CDEX ${\mathit m}_{{{\mathit A}^{0}}}$ = 1.5 keV $<1.7 \times 10^{-11}$ 90 22 ADHIKARI 2019 B C100 Solar axions $<2.3 \times 10^{-14}$ 90 23 APRILE 2019 D XE1T ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.186 - 1$ keV 24 DESSERT 2019 ASTR Magnetic white dwarf $<2.6 \times 10^{-10}$ 95 25 TERRANO 2019 Torsion pendulum $<1.5 \times 10^{-13}$ 90 26 ABE 2018 F XMAS ${\mathit m}_{{{\mathit A}^{0}}}$ = $40 - 120$ keV $<1.1 \times 10^{-11}$ 90 27 ARMENGAUD 2018 EDE3 Solar axions $<4 \times 10^{-13}$ 90 28 ARMENGAUD 2018 EDE3 ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.8 - 500$ keV $<4.9 \times 10^{-10}$ 95 29 CRESCINI 2018 QUAX ${\mathit m}_{{{\mathit A}^{0}}}$ = 58 $\mu $eV 30 FICEK 2018 THEO ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 10 keV $<4.5 \times 10^{-13}$ 90 31 ABGRALL 2017 HPGE ${\mathit m}_{{{\mathit A}^{0}}}$ = 11.8 keV $<3.5 \times 10^{-12}$ 90 32 AKERIB 2017 B LUX Solar axions $<4.2 \times 10^{-13}$ 90 33 AKERIB 2017 B LUX ${\mathit m}_{{{\mathit A}^{0}}}$ = $1 - 16$ keV $<2.3 \times 10^{-13}$ 90 34 APRILE 2017 B X100 ${\mathit m}_{{{\mathit A}^{0}}}$ = 6 keV $<4 \times 10^{-4}$ 90 35 FICEK 2017 THEO ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 1 keV $<4.35 \times 10^{-12}$ 90 36 FU 2017 A PNDX Solar axions $<4.3 \times 10^{-14}$ 90 37 FU 2017 A PNDX ${\mathit m}_{{{\mathit A}^{0}}}$ = 2 keV $<5 \times 10^{-13}$ 90 38 LIU 2017 A CDEX ${\mathit m}_{{{\mathit A}^{0}}}$ = 13 keV $<2.5 \times 10^{-11}$ 90 39 LIU 2017 A CDEX Solar axions $<0.15$ 95 40 LUO 2017 ${\mathit m}_{{{\mathit A}^{0}}}$ = 300 eV $<3.3 \times 10^{-13}$ 68 41 BATTICH 2016 ASTR White dwarf cooling $<7 \times 10^{-13}$ 42 CORSICO 2016 ASTR White dwarf cooling $<1.39 \times 10^{-11}$ 90 43 YOON 2016 KIMS Solar axions $<7.4 \times 10^{-9}$ 95 44 TERRANO 2015 ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 30 $\mu $eV $<8 \times 10^{-13}$ 90 45 ABE 2014 F XMAS ${\mathit m}_{{{\mathit A}^{0}}}$ = 60 keV $<7.7 \times 10^{-12}$ 90 46 APRILE 2014 B X100 Solar axions 47 APRILE 2014 B X100 ${\mathit m}_{{{\mathit A}^{0}}}$ = $5 - 7$ keV $< 0.96 - 8.2 \times 10^{-8}$ 90 48 DERBIN 2014 CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.1 - 1$ MeV $<2.8 \times 10^{-13}$ 99 49 MILLER-BERTOL.. 2014 ASTR White dwarf cooling $<5.4 \times 10^{-11}$ 90 50 ABE 2013 D XMAS Solar axions $<1.07 \times 10^{-12}$ 90 51 ARMENGAUD 2013 EDEL ${\mathit m}_{{{\mathit A}^{0}}}$ = 12.5 keV $<2.59 \times 10^{-11}$ 90 52 ARMENGAUD 2013 EDEL Solar axions 53 BARTH 2013 CAST Solar axions $< 1.4 - 9.7 \times 10^{-7}$ 90 54 DERBIN 2013 CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.1 - 1$ MeV $<1.5 \times 10^{-8}$ 68 55 HECKEL 2013 ${\mathit m}_{{{\mathit A}^{0}}}{}\leq{}$ 0.1 $\mu $eV $<4.3 \times 10^{-13}$ 95 56 VIAUX 2013 A ASTR Low-mass red giants $<7 \times 10^{-13}$ 95 57 CORSICO 2012 ASTR White dwarf cooling $<2.2 \times 10^{-10}$ 90 58 DERBIN 2012 CNTR Solar axions $<0.02 - 1 \times 10^{-10}$ 90 59 AALSETH 2011 CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.3 - 8$ keV $<1.4 \times 10^{-12}$ 90 60 AHMED 2009 A CDMS ${\mathit m}_{{{\mathit A}^{0}}}$ = 2.5 keV $<4 \times 10^{-9}$ 61 DAVOUDIASL 2009 ASTR Earth cooling $<2.7 \times 10^{-8}$ 66 62 NI 1994 Induced magnetism 62 CHUI 1993 Induced magnetism $<3.6 \times 10^{-7}$ 66 63 PAN 1992 Torsion pendulum $<2.9 \times 10^{-8}$ 95 62 BOBRAKOV 1991 Induced magnetism $<1.9 \times 10^{-6}$ 66 64 WINELAND 1991 NMR $<7 \times 10^{-7}$ 66 63 RITTER 1990 Torsion pendulum $<6.6 \times 10^{-8}$ 95 62 VOROBYOV 1988 Induced magnetism 1  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 ${\mathit m}_{{{\mathit A}^{0}}}$ = 0.1 keV. See their Fig. 15 for mass-dependent limits. 2  APRILE 2022B is an update of APRILE 2020 , and set the limit, $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }{ {}\lesssim{} }$ $9 \times 10^{-15} - 3 \times 10^{-13}$. The quoted limit applies to ${\mathit m}_{{{\mathit A}^{0}}}$ = 2 keV. They exclude the XENON1T excess found in APRILE 2020 . See their Fig. 6 for mass-dependent limits. 3  APRILE 2022B is an update of APRILE 2020 . They exclude the XENON1T excess found in APRILE 2020 . The quoted limit holds for small $\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }$. See their Fig. 6 for correlation between $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$ and $\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }$ . 4  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, $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }\cdot{}\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }$ $<$ $1.3 \times 10^{-25}$ GeV${}^{-1}$ at 95$\%$ CL for ${\mathit m}_{{{\mathit A}^{0}}}{ {}\lesssim{} }$ $10^{-5}$ eV. See their Fig. 1 for mass-dependent limits. 5  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 ${{\mathit \rho}_{{A}}}$ = 0.45 GeV/cm${}^{3}$ and the velocity $\mathit v$ = 220 km/sec. See their Fig. 4 for the limits. 6  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 ${\mathit m}_{{{\mathit A}^{0}}}$ = 15 MeV for the reheating temperature equal to 5 MeV. See their Fig. 2 for mass-dependent limits. 7  WANG 2022C use the spin-amplifier based on hyperpolarized ${}^{129}\mathrm {Xe}$ to set limits on the product of the axion couplings to electrons and nucleons as $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$ $\mathit g_{ {{\mathit A}} {{\mathit n}} {{\mathit n}} }$ $<$ $400$ (95 $\%$ CL) at ${\mathit m}_{{{\mathit A}^{0}}}$ = 0.1 meV. Here $\mathit g_{ {{\mathit A}} {{\mathit n}} {{\mathit n}} }$ is the dimensionless axion-neutron coupling. See their Fig. 4 for the mass-dependent limits. 8  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 $\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }$ $\mathit g_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }$ $<$ $0.4 - 2.8 \times 10^{-24}$ GeV${}^{-1}$ (95 $\%$ CL) for ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ $3.5 \times 10^{-11}$eV. 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 . 9  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. 10  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. 11  AGOSTINI 2020 is analogous to AHMED 2009A. The quoted limit applies to ${\mathit m}_{{{\mathit A}^{0}}}$ = 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. 12  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. 13  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. 14  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 $\mathit g_{ {{\mathit A}} {{\mathit N}} {{\mathit N}} }$. 15  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. 16  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. 17  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. 18  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. 19  STRANIERO 2020 is analogous to CAPOZZI 2020 , with 22 galactic globular clusters used to derive the limit. 20  WANG 2020A is an update of LIU 2017A. See their Fig. 9. 21  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. 22  ADHIKARI 2019B is analogous to LIU 2017A. 23  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. 24  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. 25  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. 26  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. 27  ARMENGAUD 2018 is analogous to LIU 2017A. 28  ARMENGAUD 2018 is analogous to AHMED 2009A. See the left panel of Fig. 5 for mass-dependent limits. 29  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${}^{3}$. 30  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. 31  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. 32  AKERIB 2017B is analogous to LIU 2017A. 33  AKERIB 2017B is analogous to AHMED 2009A. See their Fig. 7 for mass-dependent limits. 34  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. 35  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. 36  FU 2017A is analogous to LIU 2017A. See their Fig. 3 for mass-dependent limits. 37  FU 2017A is analogous to AHMED 2009A. See their Fig. 4 for mass-dependent limits. 38  LIU 2017A is analogous to AHMED 2009A. See their Fig. 9 for limits between 0.25 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 20 keV. 39  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. 40  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. 41  BATTICH 2016 is analogous to CORSICO 2016 and used the pulsating DB white dwarf PG 1351+489. 42  CORSICO 2016 studied the cooling rate of the pulsating DA white dwarf L19-2 based on an asteroseismic model. 43  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. 44  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. 45  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. 46  APRILE 2014B look for solar axions using the XENON100 detector. 47  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. 48  DERBIN 2014 is an update of DERBIN 2013 with a BGO scintillating bolometer. See their Fig. 3 for mass-dependent limits. 49  MILLER-BERTOLAMI 2014 studied the impact of axion emission on white dwarf cooling in a self-consistent way. 50  ABE 2013D is analogous to DERBIN 2012 , using the XMASS detector. 51  ARMENGAUD 2013 is similar to AALSETH 2011 . See their Fig. 10 for limits between 3 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}<$ 100 keV. 52  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. 53  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. 54  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. 55  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. 56  VIAUX 2013A constrain axion emission using the observed brightness of the tip of the red-giant branch in the globular cluster M5. 57  CORSICO 2012 attributed the excessive cooling rate of the pulsating white dwarf R548 to emission of axions with $\mathit g_{{{\mathit A}}{{\mathit e}}{{\mathit e}}}$ $\simeq{}$ $4.8 \times 10^{-13}$. 58  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. 59  AALSETH 2011 is analogous to AHMED 2009A. See their Fig.$~$4 for mass-dependent limits. 60  AHMED 2009A assume keV-mass pseudoscalars are the local dark matter and constrain the axio-electric effect in the CDMS detector. See their Fig.$~$5 for mass-dependent limits. 61  DAVOUDIASL 2009 use geophysical constraints on Earth cooling by axion emission. 62  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. 63  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. 64  WINELAND 1991 looked for an effect of bulk matter with aligned electron spins on atomic hyperfine splitting using nuclear magnetic resonance.

References:

APRILE 2022B PRL 129 161805 Search for New Physics in Electronic Recoil Data from XENONnT APRILE 2022 PR D106 022001 Emission of single and few electrons in XENON1T and limits on light dark matter DESSERT 2022 PRL 128 071102 No Evidence for Axions from Chandra Observation of the Magnetic White Dwarf RE J0317-853 IKEDA 2022 PR D105 102004 Axion search with quantum nondemolition detection of magnons LANGHOFF 2022 PRL 129 241101 Irreducible Axion Background WANG 2022C PRL 129 051801 Limits on Axions and Axionlike Particles within the Axion Window Using a Spin-Based Amplifier XIAO 2022 PR D106 123019 Betelgeuse constraints on coupling between axionlike particles and electrons CALORE 2021 PR D104 043016 Supernova bounds on axionlike particles coupled with nucleons and electrons LUCENTE 2021 PR D104 103007 Supernova bound on axionlike particles coupled with electrons 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 ADHIKARI 2019B 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