• • • We do not use the following data for averages, fits, limits, etc. • • • |
$<4 \times 10^{-5}$ |
90 |
1 |
|
PICO |
$<5 \times 10^{-4}$ |
90 |
2 |
|
XE1T |
$<7 \times 10^{-4}$ |
90 |
3 |
|
PNDX |
$<8 \times 10^{-4}$ |
90 |
4 |
|
LUX |
$<0.28$ |
90 |
5 |
|
DRFT |
$<0.027$ |
90 |
6 |
|
PICA |
$<5 \times 10^{-4}$ |
90 |
7 |
|
PICO |
$<6.8 \times 10^{-3}$ |
90 |
8 |
|
X100 |
$<6.3 \times 10^{-3}$ |
90 |
9 |
|
SMPL |
$<0.01$ |
90 |
10 |
|
ZEP3 |
$<7 \times 10^{-3}$ |
|
11 |
|
COUP |
$<8.5 \times 10^{-3}$ |
|
12 |
|
SMPL |
$<0.016$ |
90 |
13 |
|
KIMS |
$5 \times 10^{-10} \text{ to }\text{E-5}$ |
95 |
14 |
|
THEO |
$<1$ |
90 |
15 |
|
XE10 |
$<0.055$ |
|
16 |
|
HDMS |
$<0.33$ |
90 |
17 |
|
COUP |
$<5$ |
|
18 |
|
CDMS |
$<2$ |
|
19 |
|
CNTR |
$<0.4$ |
|
20 |
|
NAIA |
$<2$ |
|
21 |
|
PICA |
$2 \times 10^{-11} \text{ to 1 }\times 10^{-4}$ |
|
22 |
|
THEO |
$<0.8$ |
|
23 |
|
NAIA |
$<40$ |
|
24 |
|
BOLO |
$<10$ |
|
25 |
|
CRES |
$8 \times 10^{-7} \text{ to 2 }\times 10^{-5}$ |
|
26 |
|
THEO |
$<3.8$ |
|
27 |
|
DAMA |
$<0.8$ |
|
|
|
UKDM |
$<4.8$ |
|
28 |
|
DAMA |
$<100$ |
|
29 |
|
BOLO |
$<0.6$ |
|
|
|
DAMA |
$<5$ |
|
28 |
|
DAMA |
1
The strongest limit is $<$ $2.5 \times 10^{-5}$ pb at ${\mathit m}_{{{\mathit \chi}}}$ = 25 GeV. This updates AMOLE 2017 .
|
2
The strongest limit is $<$ $2 \times 10^{-4}$ pb at ${\mathit m}_{{{\mathit \chi}}}$ = 30 GeV. For scatterings on neutrons, the strongest limit is $<$ $6.3 \times 10^{-6}$ at ${\mathit m}_{{{\mathit \chi}}}$ = 30 GeV.
|
3
The strongest limit is $<$ $4.4 \times 10^{-4}$ pb at ${\mathit m}_{{{\mathit \chi}}}$ = 40 GeV. This updates FU 2017 .
|
4
The strongest limit is $5 \times 10^{-4}$ pb at ${\mathit m}_{{{\mathit \chi}}}$ = 35 GeV. The limit for scattering on neutrons is $3 \times 10^{-5}$ pb at 100 GeV and is $1.6 \times 10^{-5}$ pb at 35 GeV. This updates AKERIB 2016A.
|
5
Directional recoil detector. This updates DAW 2012 .
|
6
This result updates ARCHAMBAULT 2012 . The strongest limit is 0.013 pb at ${\mathit m}_{{{\mathit \chi}}}$ = 20 GeV.
|
7
The strongest limit is $5 \times 10^{-4}$ pb at ${\mathit m}_{{{\mathit \chi}}}$ = 80 GeV.
|
8
The strongest limit is $5.2 \times 10^{-3}$ pb at 50 GeV. The limit for scattering on neutrons is $2.8 \times 10^{-4}$ pb at 100 GeV and the strongest limit is $2.0 \times 10^{-4}$ pb at 50 GeV. This updates APRILE 2013 .
|
9
The strongest limit is 0.0043 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}$ = 35 GeV. FELIZARDO 2014 also presents limits for the scattering on neutrons. At ${\mathit m}_{{{\mathit \chi}}}$ = 100 GeV, the upper limit is 0.13 pb and the strongest limit is 0.066 pb at ${\mathit m}_{{{\mathit \chi}}}$ = 35 GeV.
|
10
This result updates LEBEDENKO 2009A. The strongest limit is $8 \times 10^{-3}$ pb at ${\mathit m}_{{{\mathit \chi}}}$ = 50 GeV. Limit applies to the neutralino neutron elastic cross section.
|
11
The strongest limit is $6 \times 10^{-3}$ at ${\mathit m}_{{{\mathit \chi}}}$ = 60 GeV.
|
12
The strongest limit is $5.7 \times 10^{-3}$ at ${\mathit m}_{{{\mathit \chi}}}$ = 35 GeV.
|
13
This result updates LEE 2007A. The strongest limit is at ${\mathit m}_{{{\mathit \chi}}}$ = 80 GeV.
|
14
Predictions for the spin-dependent elastic cross section based on a frequentist approach to electroweak observables in the framework of ${{\mathit N}}$ = 1 supergravity models with radiative breaking of the electroweak gauge symmetry.
|
15
The strongest limit is 0.6 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}$= 30 GeV. The limit for scattering on neutrons is 0.01 pb at ${\mathit m}_{{{\mathit \chi}}}$= 100 GeV, and the strongest limit is 0.0045 pb at ${\mathit m}_{{{\mathit \chi}}}$= 30$~$GeV.
|
16
Limit applies to neutron elastic cross section.
|
17
The strongest upper limit is 0.25 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}\simeq{}$40 GeV.
|
18
The strongest upper limit is 4 pb and occurs at ${{\mathit m}_{{\chi}}}$ $\simeq{}$ 60 GeV. The limit on the neutron spin-dependent elastic cross section is 0.07 pb. This latter limit is improved in AHMED 2009 , where a limit of 0.02 pb is obtained at ${\mathit m}_{{{\mathit \chi}}}$ = 100 GeV. The strongest limit in AHMED 2009 is 0.018 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}$ = 60 GeV.
|
19
The strongest upper limit is 1.2 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}$ $\simeq{}$ 40 GeV. The limit on the neutron spin-dependent cross section is 35 pb.
|
20
The strongest upper limit is 0.35 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}$ $\simeq{}$ 60 GeV.
|
21
The strongest upper limit is 1.2 pb and occurs ${\mathit m}_{{{\mathit \chi}}}$ $\simeq{}$ 30 GeV.
|
22
ELLIS 2004 calculates the ${{\mathit \chi}}{{\mathit p}}$ elastic scattering cross section in the framework of $\mathit N$=1 supergravity models with radiative breaking of the electroweak gauge symmetry, but without universal scalar masses. In the case of universal squark and slepton masses, but non-universal Higgs masses, the limit becomes $2 \times 10^{-4}$, see ELLIS 2003E.
|
23
The strongest upper limit is 0.75 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}\approx{}$70 GeV.
|
24
The strongest upper limit is 30 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}$ $\approx{}$ 20~GeV.
|
25
The strongest upper limit is 8 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}\simeq{}$30 GeV.
|
26
ELLIS 2001C calculates the ${{\mathit \chi}}-{{\mathit p}}$ elastic scattering cross section in the framework of $\mathit N$=1 supergravity models with radiative breaking of the electroweak gauge symmetry. In models with nonuniversal Higgs masses, the upper limit to the cross section is $6 \times 10^{-4}$.
|
27
The strongest upper limit is 3 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}\simeq{}$60 GeV. The limits are for inelastic scattering ${{\mathit X}^{0}}$ ${+}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{+}$ ${}^{129}\mathrm {Xe}^{*}$ (39.58 keV).
|
28
The strongest upper limit is 4.4 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}\simeq{}$60 GeV.
|
29
The strongest upper limit is about 35 pb and occurs at ${\mathit m}_{{{\mathit \chi}}}\simeq{}$15 GeV.
|