Cross-Section Limits for Dark Matter Particles (${{\mathit X}^{0}}$) on Nuclei

For ${\mathit m}_{{{\mathit X}^{0}}}$ = 20 GeV

INSPIRE   PDGID:
S030DM1
VALUE (nb) CL% DOCUMENT ID TECN  COMMENT
• • We do not use the following data for averages, fits, limits, etc. • •
$<0.03$ 90 1
UCHIDA
2014
XMAS ${}^{129}\mathrm {Xe}$, inelastic
$<0.08$ 90 2
ANGLOHER
2002
CRES ${}^{}\mathrm {Al}$
3
BENOIT
2000
EDEL Ge
$<0.04$ 95 4
KLIMENKO
1998
CNTR ${}^{73}\mathrm {Ge}$, inel.
$<0.8$
ALESSANDRELLO
1996
CNTR ${}^{}\mathrm {O}$
$<6$
ALESSANDRELLO
1996
CNTR ${}^{}\mathrm {Te}$
$<0.02$ 90 5
BELLI
1996
CNTR ${}^{129}\mathrm {Xe}$, inel.
6
BELLI
1996C
 CNTR ${}^{129}\mathrm {Xe}$
$<4 \times 10^{-3}$ 90 7
BERNABEI
1996
CNTR ${}^{}\mathrm {Na}$
$<0.3$ 90 7
BERNABEI
1996
CNTR ${}^{}\mathrm {I}$
$<0.2$ 95 8
SARSA
1996
CNTR ${}^{}\mathrm {Na}$
$<0.015$ 90 9
SMITH
1996
CNTR ${}^{}\mathrm {Na}$
$<0.05$ 95 10
GARCIA
1995
CNTR Natural ${}^{}\mathrm {Ge}$
$<0.1$ 95
QUENBY
1995
CNTR ${}^{}\mathrm {Na}$
$<90$ 90 11
SNOWDEN-IFFT
1995
MICA ${}^{16}\mathrm {O}$
$<4 \times 10^{3}$ 90 11
SNOWDEN-IFFT
1995
MICA ${}^{39}\mathrm {K}$
$<0.7$ 90
BACCI
1992
CNTR ${}^{}\mathrm {Na}$
$<0.12$ 90 12
REUSSER
1991
CNTR Natural ${}^{}\mathrm {Ge}$
$<0.06$ 95
CALDWELL
1988
CNTR Natural ${}^{}\mathrm {Ge}$
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  KLIMENKO 1998 limit is for inelastic scattering ${{\mathit X}^{0}}$ $~{}^{73}\mathrm {Ge}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{73}\mathrm {Ge}{}^{*}$ ($13.26$ keV).
5  BELLI 1996 limit for inelastic scattering ${{\mathit X}^{0}}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{129}\mathrm {Xe}^{*}(39.58$ keV).
6  BELLI 1996C use background subtraction and obtain $\sigma <150~$pb ($<1.5~$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.
7  BERNABEI 1996 use pulse shape discrimination to enhance the possible signal. The limit here is from R.$~$Bernabei, private communication, September 19, 1997.
8  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.
9  SMITH 1996 use pulse shape discrimination to enhance the possible signal. A dark matter density of $0.4~$GeV$~$cm${}^{-3}$ is assumed.
10  GARCIA 1995 limit is from the event rate. A weaker limit is obtained from searches for diurnal and annual modulation.
11  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.
12  REUSSER 1991 limit here is changed from published ($0.04$) after reanalysis by authors. J.L.$~$Vuilleumier, private communication, March 29, 1996.
References