The limit is for $\mathit G_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }\partial{}_{{{\mathit \mu}}}\phi _{\mathit A}{{\overline{\mathit e}}}\gamma {}^{\mu }\gamma _{5}{{\mathit e}}$ in GeV${}^{-1}$, or equivalently, the dipole-dipole potential ${\mathit G{}^{2}_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }\over 4{{\mathit \pi}}}$ (($\mathbf {\sigma }_{1}\cdot{}\mathbf {\sigma }_{2}$) $-3(\mathbf {\sigma }_{1}\cdot{}\mathbf {\mathit n}$) ($\mathbf {\sigma }_{2}\cdot{}\mathbf {\mathit n}))/\mathit r{}^{3}$ where $\mathbf {\mathit n}=\mathbf {\mathit r}/\mathit r$.

VALUE (GeV${}^{-1}$) CL% DOCUMENT ID TECN  COMMENT • • We do not use the following data for averages, fits, limits, etc. • • $<4.4 \times 10^{-10}$ 90 1 ABGRALL 2017 HPGE ${\mathit m}_{{{\mathit A}^{0}}}$ = 11.8 keV $<3.4 \times 10^{-9}$ 90 2 AKERIB 2017 B LUX Solar axions $<4.1 \times 10^{-10}$ 90 3 AKERIB 2017 B LUX ${\mathit m}_{{{\mathit A}^{0}}}$ = $1 - 16$ keV $<2 \times 10^{-10}$ 90 4 APRILE 2017 B X100 ${\mathit m}_{{{\mathit A}^{0}}}$ = 6 keV $<5 \times 10^{-10}$ 90 5 LIU 2017 A CDEX ${\mathit m}_{{{\mathit A}^{0}}}$ = 13 keV $<2.5 \times 10^{-8}$ 90 6 LIU 2017 A CDEX Solar axions $<3.2 \times 10^{-10}$ 68 7 BATTICH 2016 ASTR White dwarf cooling $<7 \times 10^{-10}$ 8 CORSICO 2016 ASTR White dwarf cooling $<1.36 \times 10^{-8}$ 90 9 YOON 2016 KIMS Solar axions $<7.3 \times 10^{-6}$ 95 10 TERRANO 2015 ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 30 $\mu $eV $<7.8 \times 10^{-10}$ 90 11 ABE 2014 F XMAS ${\mathit m}_{{{\mathit A}^{0}}}$ = 60 keV $<7.5 \times 10^{-9}$ 90 12 APRILE 2014 B X100 Solar axions 13 APRILE 2014 B X100 ${\mathit m}_{{{\mathit A}^{0}}}$ = $5 - 7$ keV $< 0.94 - 8.0 \times 10^{-5}$ 90 14 DERBIN 2014 CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.1 - 1$ MeV $<3 \times 10^{-10}$ 99 15 MILLER-BERTOL.. 2014 ASTR White dwarf cooling $<5.3 \times 10^{-8}$ 90 16 ABE 2013 D XMAS Solar axions $<1.05 \times 10^{-9}$ 90 17 ARMENGAUD 2013 EDEL ${\mathit m}_{{{\mathit A}^{0}}}$ = 12.5 keV $<2.53 \times 10^{-8}$ 90 18 ARMENGAUD 2013 EDEL Solar axions 19 BARTH 2013 CAST Solar axions $< 1.4 - 9.5 \times 10^{-4}$ 90 20 DERBIN 2013 CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.1 - 1$ MeV $<2.9 \times 10^{-5}$ 68 21 HECKEL 2013 ${\mathit m}_{{{\mathit A}^{0}}}{}\leq{}$ 0.1 $\mu $eV $<4.2 \times 10^{-10}$ 95 22 VIAUX 2013 A ASTR Low-mass red giants $<7 \times 10^{-10}$ 95 23 CORSICO 2012 ASTR White dwarf cooling $<2.2 \times 10^{-7}$ 90 24 DERBIN 2012 CNTR Solar axions $<0.02 - 1 \times 10^{-7}$ 90 25 AALSETH 2011 CNTR ${\mathit m}_{{{\mathit A}^{0}}}$ = $0.3 - 8$ keV $<1.4 \times 10^{-9}$ 90 26 AHMED 2009 A CDMS ${\mathit m}_{{{\mathit A}^{0}}}$ = 2.5 keV $<3 \times 10^{-6}$ 27 DAVOUDIASL 2009 ASTR Earth cooling $<5.3 \times 10^{-5}$ 66 28 NI 1994 Induced magnetism $<6.7 \times 10^{-5}$ 66 28 CHUI 1993 Induced magnetism $<3.6 \times 10^{-4}$ 66 29 PAN 1992 Torsion pendulum $<2.7 \times 10^{-5}$ 95 28 BOBRAKOV 1991 Induced magnetism $<1.9 \times 10^{-3}$ 66 30 WINELAND 1991 NMR $<8.9 \times 10^{-4}$ 66 29 RITTER 1990 Torsion pendulum $<6.6 \times 10^{-5}$ 95 28 VOROBYOV 1988 Induced magnetism 1  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. 2  AKERIB 2017B is analogous to LIU 2017A. 3  AKERIB 2017B is analogous to AHMED 2009A. See their Fig. 7 for mass-dependent limits. 4  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. 5  LIU 2017A is analogous to AHMED 2009A. See their Fig. 9 for limits between 0.25 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 20 keV. 6  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. 7  BATTICH 2016 is analogous to CORSICO 2016 and used the pulsating DB white dwarf PG 1351+489. 8  CORSICO 2016 studied the cooling rate of the pulsating DA white dwarf L19-2 based on an asteroseismic model. 9  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. 10  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. 11  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. 12  APRILE 2014B look for solar axions using the XENON100 detector. 13  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. 14  DERBIN 2014 is an update of DERBIN 2013 with a BGO scintillating bolometer. See their Fig. 3 for mass-dependent limits. 15  MILLER-BERTOLAMI 2014 studied the impact of axion emission on white dwarf cooling in a self-consistent way. 16  ABE 2013D is analogous to DERBIN 2012 , using the XMASS detector. 17  ARMENGAUD 2013 is similar to AALSETH 2011 . See their Fig. 10 for limits between 3 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}<$ 100 keV. 18  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. 19  BARTH 2013 search for solar axions produced by axion-electron coupling, and obtained the limit, $\mathit G_{ {{\mathit A}} {{\mathit e}} {{\mathit e}} }\cdot{}\mathit G_{ {{\mathit A}} {{\mathit \gamma}} {{\mathit \gamma}} }<$ $7.9 \times 10^{-20}$ GeV${}^{-2}$ at 95$\%$CL. 20  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. 21  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. 22  VIAUX 2013A constrain axion emission using the observed brightness of the tip of the red-giant branch in the globular cluster M5. 23  CORSICO 2012 attributed the excessive cooling rate of the pulsating white dwarf R548 to emission of axions with $\mathit G_{{{\mathit A}}{{\mathit e}}{{\mathit e}}}$ $\simeq{}$ $5 \times 10^{-10}$. 24  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. 25  AALSETH 2011 is analogous to AHMED 2009A. See their Fig.$~$4 for mass-dependent limits. 26  AHMED 2009A assume keV-mass pseudoscalars are the local dark matter and constrain the axio-electric effect in the CDMS detector. See their Fig.$~$5 for mass-dependent limits. 27  DAVOUDIASL 2009 use geophysical constraints on Earth cooling by axion emission. 28  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. 29  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. 30  WINELAND 1991 looked for an effect of bulk matter with aligned electron spins on atomic hyperfine splitting using nuclear magnetic resonance.

References:

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