| • • • We do not use the following data for averages, fits, limits, etc. • • • |
| $<0.03$ |
|
1 |
|
ASTR |
| $<9.6 \times 10^{-3}$ |
95 |
2 |
|
ASTR |
|
|
3 |
|
|
|
|
4 |
|
NMR |
| $<65$ |
95 |
5 |
|
CNTR |
| $<6.6$ |
90 |
6 |
|
EDE3 |
| $<0.085$ |
90 |
7 |
|
ASTR |
| $<12.7$ |
95 |
8 |
|
CNTR |
| $<0.01$ |
|
9 |
|
ASTR |
|
|
10 |
|
|
| $<93$ |
90 |
11 |
|
HPGE |
| $<4$ |
90 |
12 |
|
PNDX |
|
|
13 |
|
|
| $<177$ |
90 |
14 |
|
CDEX |
| $<0.079$ |
95 |
15 |
|
ASTR |
| $< 100$ |
95 |
16 |
|
CNTR |
|
|
17 |
|
|
|
|
18 |
|
|
|
|
19 |
|
|
|
|
20 |
|
|
|
|
21 |
|
|
|
|
22 |
|
COSM |
|
|
23 |
|
ASTR |
| $<250$ |
95 |
24 |
|
CNTR |
| $<155$ |
90 |
25 |
|
EDEL |
| $<8.6 \times 10^{3}$ |
90 |
26 |
|
CNTR |
| $<1.4 \times 10^{4}$ |
90 |
27 |
|
BORX |
| $<145$ |
95 |
28 |
|
CNTR |
|
|
29 |
|
CNTR |
|
|
30 |
|
|
|
1
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 $\mathit g_{Ann}$ $<$ $1.0 \times 10^{-10}$.
|
|
2
LLOYD 2019 is analogous to BERENJI 2016 . They highlight that the limit obtained with this technique strongly depends on the assumed NS core temperature.
|
|
3
SMORRA 2019 look for spin-precession effects from ultra-light axion dark matter in the ${{\overline{\mathit p}}}$ spin-flip resonance data. Assuming ${{\mathit \rho}_{{A}}}$ = 0.4 GeV/cm${}^{3}$, they constrain the dimensionless axion-antiproton coupling as $\mathit g_{ {{\mathit A}} {{\overline{\mathit p}}} {{\overline{\mathit p}}} }$ $<$ $2 - 9$ at 95$\%$ CL for ${\mathit m}_{{{\mathit A}^{0}}}$ = $2 \times 10^{-23} - 4 \times 10^{-17}$ eV. See the right panel of their Fig. 3.
|
|
4
WU 2019 look for axion-induced time-oscillating features of the NMR spectrum of acetonitrile-2-${}^{13}\mathrm {C}$. Assuming C$_{p}$ = C$_{n}$ and ${{\mathit \rho}_{{A}}}$ = 0.4 GeV/cm${}^{3}$, they constrain the dimensionless axion-nucleon coupling as ${{\mathit g}_{{ANN}}}$ $<$ $6 \times 10^{-5}$ for ${\mathit m}_{{{\mathit A}^{0}}}$ = $10^{-21} - 1.3 \times 10^{-17}$ eV. Note that the limits for ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ $10^{-21}$ eV in their Fig. 3(a) should be weaker than those for heavier masses. See ADELBERGER 2019 and WU 2019C on this issue.
|
|
5
AKHMATOV 2018 is an update of GAVRILYUK 2015 .
|
|
6
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.
|
|
7
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 $\mathit g_{Ann}$ $<$ $2.8 \times 10^{-10}$.
|
|
8
GAVRILYUK 2018 look for the resonant excitation of ${}^{83}\mathrm {Kr}$ (9.4 keV) by solar axions produced via the Primakoff effect. The mass bound assumes ${\mathit m}_{{{\mathit u}}}/{\mathit m}_{{{\mathit d}}}$ = 0.56 and $\mathit S$ = 0.5.
|
|
9
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 $\mathit f_{A}$ $>$ $5 \times 10^{8}$ GeV obtained for the KSVZ axion with C$_{p}$ = $-0.47$ and C$_{n}$ = $-0.02$.
|
|
10
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 ${\mathit m}_{{{\mathit A}^{0}}}$ = $10^{-24} - 10^{-17}$ eV.
|
|
11
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.
|
|
12
FU 2017A look for the 14.4 keV ${}^{57}\mathrm {Fe}$ 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.
|
|
13
KLIMCHITSKAYA 2017A use the differential measurement of the Casimir force between a ${}^{}\mathrm {Ni}$-coated sphere and ${}^{}\mathrm {Au}$ and ${}^{}\mathrm {Ni}$ sectors of the structured disc to constrain the axion coupling to nucleons for $2.61$ meV $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 0.9 eV. See their Figs. 1 and 2 for mass dependent limits.
|
|
14
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.
|
|
15
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.
|
|
16
GAVRILYUK 2015 look for solar axions emitted by the M1 transition of ${}^{83}\mathrm {Kr}$ (9.4 keV). The mass bound assumes ${\mathit m}_{{{\mathit u}}}/{\mathit m}_{{{\mathit d}}}$ = 0.56 and $\mathit S$ = 0.5.
|
|
17
KLIMCHITSKAYA 2015 use the measurement of differential forces between a test mass and rotating source masses of ${}^{}\mathrm {Au}$ and ${}^{}\mathrm {Si}$ to constrain the force due to two-axion exchange for $1.7 \times 10^{-3}$ $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 0.9 eV. See their Figs. 1 and 2 for mass dependent limits.
|
|
18
BEZERRA 2014 use the measurement of the thermal Casimir-Polder force between a Bose-Einstein condensate of ${}^{87}\mathrm {Rb}$ atoms and a ${}^{}\mathrm {SiO}_{2}$ plate to constrain the force mediated by exchange of two pseudoscalars for 0.1 meV $<$ ${\mathit m}_{{{\mathit A}^{0}}}<$ 0.3 eV. See their Fig. 2 for the mass-dependent limit on pseudoscalar coupling to nucleons.
|
|
19
BEZERRA 2014A is analogous to BEZERRA 2014 . They use the measurement of the Casimir pressure between two ${}^{}\mathrm {Au}$-coated plates to constrain pseudoscalar coupling to nucleons for $1 \times 10^{-3}$ eV $<$ ${\mathit m}_{{{\mathit A}^{0}}}<$ 15 eV. See their Figs. 1 and 2 for the mass-dependent limit.
|
|
20
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 $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 20 eV. See their Figs. $1 - 3$ for mass-dependent limits.
|
|
21
BEZERRA 2014C is analogous to BEZERRA 2014 . They use the measurement of the gradient of the Casimir force between ${}^{}\mathrm {Au}$- and ${}^{}\mathrm {Ni}$-coated surfaces of a sphere and a plate to constrain pseudoscalar coupling to nucleons for $3 \times 10^{-5}$ eV $<$ ${\mathit m}_{{{\mathit A}_{{0}}}}$ $<$ 1 eV. See their Figs. 1, 3, and 4 for the mass-dependent limits.
|
|
22
BLUM 2014 studied effects of an oscillating strong $\mathit CP$ phase induced by axion dark matter on the primordial ${}^{4}\mathrm {He}$ abundance. See their Fig. 1 for mass-dependent limits.
|
|
23
LEINSON 2014 attributes the excessive cooling rate of the neutron star in Cassiopeia A to axion emission from the superfluid core, and found C${}^{2}_{n}{{\mathit m}^{2}}_{{{\mathit A}^{0}}}$ $\simeq{}$ $5.7 \times 10^{-6}$ eV${}^{2}$, where C$_{n}$ is the effective Peccei-Quinn charge of the neutron.
|
|
24
ALESSANDRIA 2013 used the CUORE experiment to look for 14.4 keV solar axions produced from the M1 transition of thermally excited ${}^{57}\mathrm {Fe}$ 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.
|
|
25
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.
|
|
26
BELLI 2012 looked for solar axions emitted by the M1 transition of ${}^{7}\mathrm {Li}{}^{*}$ (478 keV) after the electron capture of ${}^{7}\mathrm {Be}$, using the resonant excitation ${}^{7}\mathrm {Li}$ in the ${}^{}\mathrm {LiF}$ crystal. The mass bound assumes ${\mathit m}_{{{\mathit u}}}/{\mathit m}_{{{\mathit d}}}$ = 0.55, ${\mathit m}_{{{\mathit u}}}/{\mathit m}_{{{\mathit s}}}$ = 0.029, and the flavor-singlet axial vector matrix element $\mathit S$ = 0.4.
|
|
27
BELLINI 2012B looked for 5.5 MeV solar axions produced in the ${{\mathit p}}$ ${{\mathit d}}$ $\rightarrow$ ${}^{3}\mathrm {He}{{\mathit A}^{0}}$.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.
|
|
28
DERBIN 2011 looked for solar axions emitted by the M1 transition of thermally excited ${}^{57}\mathrm {Fe}$ nuclei in the Sun, using their possible resonant capture on ${}^{57}\mathrm {Fe}$ in the laboratory. The mass bound assumes ${\mathit m}_{{{\mathit u}}}/{\mathit m}_{{{\mathit d}}}$ = 0.56 and the flavor-singlet axial vector matrix element ${{\mathit S}}$ = 3${{\mathit F}}−{{\mathit D}}$ $\simeq{}$ 0.5.
|
|
29
BELLINI 2008 consider solar axions emitted in the M1 transition of ${}^{7}\mathrm {Li}{}^{*}$ (478 keV) and look for a peak at 478 keV in the energy spectra of the Counting Test Facility (CTF), a Borexino prototype. For ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 450 keV they find mass-dependent limits on products of axion couplings to photons, electrons, and nucleons.
|
|
30
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 ${\mathit m}_{{{\mathit A}^{0}}}$ below about 1 meV.
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