| • • • We do not use the following data for averages, fits, limits, etc. • • • |
| $<0.03$ |
90 |
1 |
|
XMAS |
| $<3$ |
90 |
2 |
|
CRES |
|
|
3 |
|
EDEL |
|
|
4 |
|
CNTR |
|
|
5 |
|
CNTR |
| $<0.06$ |
95 |
6 |
|
CNTR |
| $<0.4$ |
95 |
7 |
|
CNTR |
| $<40$ |
|
|
|
CNTR |
| $<700$ |
|
|
|
CNTR |
| $<0.05$ |
90 |
8 |
|
CNTR |
| $<1.5$ |
90 |
9 |
|
CNTR |
|
|
10 |
|
CNTR |
| $<0.01$ |
90 |
11 |
|
CNTR |
| $<9$ |
90 |
11 |
|
CNTR |
| $<7$ |
95 |
12 |
|
CNTR |
| $<0.3$ |
90 |
13 |
|
CNTR |
| $<6$ |
90 |
13 |
|
CNTR |
| $<6$ |
95 |
14 |
|
CNTR |
| $<8$ |
95 |
|
|
CNTR |
| $<50$ |
95 |
|
|
CNTR |
| $<700$ |
90 |
15 |
|
MICA |
| $<1 \times 10^{3}$ |
90 |
15 |
|
MICA |
| $<0.8$ |
90 |
16 |
|
CNTR |
| $<30$ |
90 |
|
|
CNTR |
| $<30$ |
90 |
|
|
CNTR |
| $<15$ |
90 |
17 |
|
CNTR |
| $<6$ |
95 |
|
|
CNTR |
|
1
UCHIDA 2014 limit is for inelastic scattering ${{\mathit X}^{0}}$ ${+}$ ${}^{129}\mathrm {Xe}^{*}$ $\rightarrow$ ${{\mathit X}^{0}}{+}$ ${}^{129}\mathrm {Xe}^{*}$ (39.58 keV).
|
|
2
ANGLOHER 2002 limit is for spin-dependent WIMP-Aluminum cross section.
|
|
3
BENOIT 2000 find four event categories in Ge detectors and suggest that low-energy surface nuclear recoils can explain anomalous events reported by UKDMC and Saclay NaI experiments.
|
|
4
BERNABEI 1999D search for SIMPs (Strongly Interacting Massive Particles) in the mass range $10^{3} - 10^{16}$ GeV. See their Fig.$~$3 for cross-section limits.
|
|
5
DERBIN 1999 search for SIMPs (Strongly Interacting Massive Particles) in the mass range GeV. See their Fig.$~$3 for cross-section limits.
|
|
6
KLIMENKO 1998 limit is for inelastic scattering ${{\mathit X}^{0}}$ $~{}^{73}\mathrm {Ge}$ $\rightarrow$ ${{\mathit X}^{0}}$ ${}^{73}\mathrm {Ge}{}^{*}$ ($13.26$ keV).
|
|
7
KLIMENKO 1998 limit is for inelastic scattering ${{\mathit X}^{0}}$ $~{}^{73}\mathrm {Ge}$ $\rightarrow$ ${{\mathit X}^{0}}$ ${}^{73}\mathrm {Ge}{}^{*}$ ($66.73$ keV).
|
|
8
BELLI 1996 limit for inelastic scattering ${{\mathit X}^{0}}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{129}\mathrm {Xe}^{*}(39.58$ keV).
|
|
9
BELLI 1996 limit for inelastic scattering ${{\mathit X}^{0}}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{129}\mathrm {Xe}^{*}(236.14$ keV).
|
|
10
BELLI 1996C use background subtraction and obtain $\sigma <0.7~$pb ($<0.7~$fb) (90$\%$ CL) for spin-dependent (independent) ${{\mathit X}^{0}}$-proton cross section. The confidence level is from R. Bernabei, private communication, May 20, 1999.
|
|
11
BERNABEI 1996 use pulse shape discrimination to enhance the possible signal. The limit here is from R.$~$Bernabei, private communication, September 19, 1997.
|
|
12
SARSA 1996 search for annual modulation of WIMP signal. See SARSA 1997 for details of the analysis. The limit here is from M.L.$~$Sarsa, private communication, May 26, 1997.
|
|
13
SMITH 1996 use pulse shape discrimination to enhance the possible signal. A dark matter density of $0.4~$GeV$~$cm${}^{-3}$ is assumed.
|
|
14
GARCIA 1995 limit is from the event rate. A weaker limit is obtained from searches for diurnal and annual modulation.
|
|
15
SNOWDEN-IFFT 1995 look for recoil tracks in an ancient mica crystal. Similar limits are also given for ${}^{27}\mathrm {Al}$ and ${}^{28}\mathrm {Si}$. See COLLAR 1996 and SNOWDEN-IFFT 1996 for discussion on potential backgrounds.
|
|
16
BECK 1994 uses enriched ${}^{76}\mathrm {Ge}$ (86$\%$ purity).
|
|
17
REUSSER 1991 limit here is changed from published ($5$) after reanalysis by authors. J.L.$~$Vuilleumier, private communication, March 29, 1996.
|
