| • • • We do not use the following data for averages, fits, limits, etc. • • • |
| $<3.2 \times 10^{-10}$ |
68 |
1 |
|
ASTR |
| $<7 \times 10^{-10}$ |
|
2 |
|
ASTR |
| $<1.36 \times 10^{-8}$ |
90 |
3 |
|
KIMS |
| $<7.3 \times 10^{-6}$ |
95 |
4 |
|
|
| $<7.8 \times 10^{-10}$ |
90 |
5 |
|
XMAS |
| $<7.5 \times 10^{-9}$ |
90 |
6 |
|
X100 |
| $<1 \times 10^{-9}$ |
90 |
7 |
|
X100 |
| $\text{< 0.94 - 8.0}$ |
90 |
8 |
|
CNTR |
| $<3 \times 10^{-10}$ |
99 |
9 |
|
ASTR |
| $<5.3 \times 10^{-8}$ |
90 |
10 |
|
XMAS |
| $<1.05 \times 10^{-9}$ |
90 |
11 |
|
EDEL |
| $<2.53 \times 10^{-8}$ |
90 |
12 |
|
EDEL |
|
|
13 |
|
CAST |
| $\text{< 1.4 - 9.5}$ |
90 |
14 |
|
CNTR |
| $<2.9 \times 10^{-5}$ |
68 |
15 |
|
|
| $<4.2 \times 10^{-10}$ |
95 |
16 |
|
ASTR |
| $<7 \times 10^{-10}$ |
95 |
17 |
|
ASTR |
| $<2.2 \times 10^{-7}$ |
90 |
18 |
|
CNTR |
| $\text{<0.02 - 1}$ |
90 |
19 |
|
CNTR |
| $<1.4 \times 10^{-9}$ |
90 |
20 |
|
CDMS |
| $<3 \times 10^{-6}$ |
|
21 |
|
ASTR |
| $<5.3 \times 10^{-5}$ |
66 |
22 |
|
|
| $<6.7 \times 10^{-5}$ |
66 |
22 |
|
|
| $<3.6 \times 10^{-4}$ |
66 |
23 |
|
|
| $<2.7 \times 10^{-5}$ |
95 |
22 |
|
|
| $<1.9 \times 10^{-3}$ |
66 |
24 |
|
NMR |
| $<8.9 \times 10^{-4}$ |
66 |
23 |
|
|
| $<6.6 \times 10^{-5}$ |
95 |
22 |
|
|
|
1
BATTICH 2016 is analogous to CORSICO 2016 and used the pulsating DB white dwarf PG 1351+489.
|
|
2
CORSICO 2016 studied the cooling rate of the pulsating DA white dwarf L19-2 based on an asteroseismic model.
|
|
3
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.
|
|
4
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.
|
|
5
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.
|
|
6
APRILE 2014B look for solar axions using the XENON100 detector.
|
|
7
APRILE 2014B is analogous to AHMED 2009A. See their Fig. 7 for limits between 1 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 35 keV.
|
|
8
DERBIN 2014 is an update of DERBIN 2013 with a BGO scintillating bolometer. See their Fig. 3 for mass-dependent limits.
|
|
9
MILLER-BERTOLAMI 2014 studied the impact of axion emission on white dwarf cooling in a self-consistent way.
|
|
10
ABE 2013D is analogous to DERBIN 2012 , using the XMASS detector.
|
|
11
ARMENGAUD 2013 is similar to AALSETH 2011 . See their Fig. 10 for limits between 3 keV $<$ ${\mathit m}_{{{\mathit A}^{0}}}<$ 100 keV.
|
|
12
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.
|
|
13
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.
|
|
14
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.
|
|
15
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.
|
|
16
VIAUX 2013A constrain axion emission using the observed brightness of the tip of the red-giant branch in the globular cluster M5.
|
|
17
CORSICO 2012 attributed the excessive cooling rate of the pulsating white dwarf R548 to emission of axions with $\mathit G_{{{\mathit A}}{{\mathit e}}{{\mathit e}}}$ $\simeq{}$ $5 \times 10^{-10}$.
|
|
18
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.
|
|
19
AALSETH 2011 is analogous to AHMED 2009A. See their Fig.$~$4 for mass-dependent limits.
|
|
20
AHMED 2009A assume keV-mass pseudoscalars are the local dark matter and constrain the axio-electric effect in the CDMS detector. See their Fig.$~$5 for mass-dependent limits.
|
|
21
DAVOUDIASL 2009 use geophysical constraints on Earth cooling by axion emission.
|
|
22
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.
|
|
23
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.
|
|
24
WINELAND 1991 looked for an effect of bulk matter with aligned electron spins on atomic hyperfine splitting using nuclear magnetic resonance.
|
