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

For ${\mathit m}_{{{\mathit X}^{0}}}$ = 100 GeV

VALUE (nb)

CL%

DOCUMENT ID

TECN

COMMENT

• • We do not use the following data for averages, fits, limits, etc. • •

$<3.3 \times 10^{-6}$

90

XE1T

${}^{129}\mathrm {Xe}$, inelastic

$<3 \times 10^{-3}$

90

XMAS

${}^{129}\mathrm {Xe}$, inelastic

$<0.3$

90

CRES

${}^{}\mathrm {Al}$

RVUE

DAMA

RVUE

RVUE

EDEL

Ge

$<4 \times 10^{-3}$

90

${}^{129}\mathrm {Xe}$, inelastic

MCRO

RVUE

$<8 \times 10^{-3}$

95

CNTR

${}^{73}\mathrm {Ge}$, inelastic

$<0.08$

95

CNTR

${}^{73}\mathrm {Ge}$, inelastic

$<4$

CNTR

${}^{}\mathrm {O}$

$<25$

CNTR

${}^{}\mathrm {Te}$

$<6 \times 10^{-3}$

90

CNTR

${}^{129}\mathrm {Xe}$, inelastic

CNTR

${}^{129}\mathrm {Xe}$

$<1 \times 10^{-3}$

90

CNTR

${}^{}\mathrm {Na}$

$<0.3$

90

CNTR

${}^{}\mathrm {I}$

$<0.7$

95

CNTR

${}^{}\mathrm {Na}$

$<0.03$

90

CNTR

${}^{}\mathrm {Na}$

$<0.8$

90

CNTR

${}^{}\mathrm {I}$

$<0.35$

95

CNTR

Natural ${}^{}\mathrm {Ge}$

$<0.6$

95

CNTR

${}^{}\mathrm {Na}$

$<3$

95

CNTR

${}^{}\mathrm {I}$

$<150$

90

MICA

${}^{16}\mathrm {O}$

$<400$

90

MICA

${}^{39}\mathrm {K}$

$<0.08$

90

CNTR

${}^{76}\mathrm {Ge}$

$<2.5$

90

CNTR

${}^{}\mathrm {Na}$

$<3$

90

CNTR

${}^{}\mathrm {I}$

$<0.9$

90

CNTR

Natural ${}^{}\mathrm {Ge}$

$<0.7$

95

CNTR

Natural ${}^{}\mathrm {Ge}$

¹	APRILE 2021A search for inelastic DM scatter off ${}^{129}\mathrm {Xe}$ nuclei with 0.83 t yr exposure. No signal obseved. Limits placed in ${{\mathit \sigma}}({{\mathit \chi}}{}^{}\mathrm {Xe}$) vs. m(DM) plane for WIMP mass between 20 GeV and 10 TeV.

²	UCHIDA 2014 limit is for inelastic scattering ${{\mathit X}^{0}}$ ${+}$ ${}^{129}\mathrm {Xe}^{}$ $\rightarrow$ ${{\mathit X}^{0}}{+}$ ${}^{129}\mathrm {Xe}^{}$(39.58 keV).

³	ANGLOHER 2002 limit is for spin-dependent WIMP-Aluminum cross section.

⁴	BELLI 2002 discuss dependence of the extracted WIMP cross section on the assumptions of the galactic halo structure.

⁵	BERNABEI 2002C analyze the DAMA data in the scenario in which ${{\mathit X}^{0}}$ scatters into a slightly heavier state as discussed by SMITH 2001.

⁶	GREEN 2002 discusses dependence of extracted WIMP cross section limits on the assumptions of the galactic halo structure.

⁷	ULLIO 2001 disfavor the possibility that the BERNABEI 1999 signal is due to spin-dependent WIMP coupling.

⁸	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.

⁹	BERNABEI 2000D limit is for inelastic scattering ${{\mathit X}^{0}}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{129}\mathrm {Xe}$ (39.58 keV).

¹⁰	AMBROSIO 1999 search for upgoing muon events induced by neutrinos originating from WIMP annihilations in the Sun and Earth.

¹¹	BRHLIK 1999 discuss the effect of astrophysical uncertainties on the WIMP interpretation of the BERNABEI 1999 signal.

¹²	KLIMENKO 1998 limit is for inelastic scattering ${{\mathit X}^{0}}$ $~{}^{73}\mathrm {Ge}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{73}\mathrm {Ge}{}^{*}$ ($13.26$ keV).

¹³	KLIMENKO 1998 limit is for inelastic scattering ${{\mathit X}^{0}}$ $~{}^{73}\mathrm {Ge}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{73}\mathrm {Ge}{}^{*}$ ($66.73$ keV).

¹⁴	BELLI 1996 limit for inelastic scattering ${{\mathit X}^{0}}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{129}\mathrm {Xe}^{*}(39.58$ keV).

¹⁵	BELLI 1996C use background subtraction and obtain $\sigma <0.35~$pb ($<0.15~$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.

¹⁶	BERNABEI 1996 use pulse shape discrimination to enhance the possible signal. The limit here is from R.$~$Bernabei, private communication, September 19, 1997.

¹⁷	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.

¹⁸	SMITH 1996 use pulse shape discrimination to enhance the possible signal. A dark matter density of $0.4~$GeV$~$cm${}^{-3}$ is assumed.

¹⁹	GARCIA 1995 limit is from the event rate. A weaker limit is obtained from searches for diurnal and annual modulation.

²⁰	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.

²¹	BECK 1994 uses enriched ${}^{76}\mathrm {Ge}$ (86$\%$ purity).

²²	REUSSER 1991 limit here is changed from published ($0.3$) after reanalysis by authors. J.L.$~$Vuilleumier, private communication, March 29, 1996.

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