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

For ${\mathit m}_{{{\mathit X}^{0}}}$ = 1 TeV

INSPIRE JSON (beta) PDGID:

VALUE (nb)

CL%

DOCUMENT ID

TECN

COMMENT

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

$<0.03$

90

XMAS

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

$<3$

90

CRES

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

EDEL

Ge

CNTR

SIMP

CNTR

SIMP

$<0.06$

95

CNTR

${}^{73}\mathrm {Ge}$, inel.

$<0.4$

95

CNTR

${}^{73}\mathrm {Ge}$, inel.

$<40$

CNTR

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

$<700$

CNTR

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

$<0.05$

90

CNTR

${}^{129}\mathrm {Xe}$, inel.

$<1.5$

90

CNTR

${}^{129}\mathrm {Xe}$, inel.

CNTR

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

$<0.01$

90

CNTR

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

$<9$

90

CNTR

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

$<7$

95

CNTR

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

$<0.3$

90

CNTR

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

$<6$

90

CNTR

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

$<6$

95

CNTR

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

$<8$

95

CNTR

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

$<50$

95

CNTR

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

$<700$

90

MICA

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

$<1 \times 10^{3}$

90

MICA

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

$<0.8$

90

CNTR

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

$<30$

90

CNTR

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

$<30$

90

CNTR

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

$<15$

90

CNTR

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

$<6$

95

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	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 $10^{2} - 10^{14}$ 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.

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