# For ${\boldsymbol m}_{{{\boldsymbol X}^{0}}}$ = 1 TeV INSPIRE search

VALUE (nb) CL% DOCUMENT ID TECN  COMMENT
• • • We do not use the following data for averages, fits, limits, etc. • • •
$<0.03$ 90 1
 2014
XMAS ${}^{129}\mathrm {Xe}$, inelastic
$<3$ 90 2
 2002
CRES ${}^{}\mathrm {Al}$
3
 2000
EDEL Ge
4
 1999 D
CNTR SIMP
5
 1999
CNTR SIMP
$<0.06$ 95 6
 1998
CNTR ${}^{73}\mathrm {Ge}$, inel.
$<0.4$ 95 7
 1998
CNTR ${}^{73}\mathrm {Ge}$, inel.
$<40$
 1996
CNTR ${}^{}\mathrm {O}$
$<700$
 1996
CNTR ${}^{}\mathrm {Te}$
$<0.05$ 90 8
 1996
CNTR ${}^{129}\mathrm {Xe}$, inel.
$<1.5$ 90 9
 1996
CNTR ${}^{129}\mathrm {Xe}$, inel.
10
 1996 C
CNTR ${}^{129}\mathrm {Xe}$
$<0.01$ 90 11
 1996
CNTR ${}^{}\mathrm {Na}$
$<9$ 90 11
 1996
CNTR ${}^{}\mathrm {I}$
$<7$ 95 12
 1996
CNTR ${}^{}\mathrm {Na}$
$<0.3$ 90 13
 1996
CNTR ${}^{}\mathrm {Na}$
$<6$ 90 13
 1996
CNTR ${}^{}\mathrm {I}$
$<6$ 95 14
 1995
CNTR Natural ${}^{}\mathrm {Ge}$
$<8$ 95
 1995
CNTR ${}^{}\mathrm {Na}$
$<50$ 95
 1995
CNTR ${}^{}\mathrm {I}$
$<700$ 90 15
 1995
MICA ${}^{16}\mathrm {O}$
$<1 \times 10^{3}$ 90 15
 1995
MICA ${}^{39}\mathrm {K}$
$<0.8$ 90 16
 1994
CNTR ${}^{76}\mathrm {Ge}$
$<30$ 90
 1992
CNTR ${}^{}\mathrm {Na}$
$<30$ 90
 1992
CNTR ${}^{}\mathrm {I}$
$<15$ 90 17
 1991
CNTR Natural ${}^{}\mathrm {Ge}$
$<6$ 95
 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  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.
References:
 UCHIDA 2014
PTEP 2014 063C01 Search for Inelastic WIMP Nucleus Scattering on ${}^{129}\mathrm {Xe}$ in Data from the XMASS-I Experiment
 ANGLOHER 2002
ASP 18 43 Limits on WIMP Dark Matter using SAPPHIRE Cryogenic Detectors
 BENOIT 2000
PL B479 8 Event Categories in the EDELWEISS WIMP Search Experiment
 BERNABEI 1999D
PRL 83 4918 Extended Limits on Neutral Strongly Interacting Massive Particles and Nuclearites from NaI(Tl) Scintillators
 DERBIN 1999
PAN 62 1886 Searches for Strongly Interacting Massive Particles by Means of Semiconductor Detectors Positioned on the Earth's Surface
 KLIMENKO 1998
JETPL 67 875 Search for Inelastic Interactions of WIMP with Excitation of ${}^{73}\mathrm {Ge}$ Nuclei
 ALESSANDRELLO 1996
PL B384 316 Preliminary Results on the Performance of a TeO$_{2}$ Thermal Detector in a Search for Direct Interactions of WIMPs
 BELLI 1996
PL B387 222 Limits on WIMP $−$ ${}^{129}\mathrm {Xe}$ Inelastic Scattering
 BELLI 1996C
NC C19 537 Search for WIMPs with Enriched Xenon at Gran Sasso
 BERNABEI 1996
PL B389 757 New Limits on WIMP Search with Large Mass Low Radioactivity Nai(Tl) Setup at Gran Sasso
 SARSA 1996
PL B386 458 Searching for Annual Modulation of WIMPs with NaI Scintillators
 SMITH 1996
PL B379 299 Improved Dark Matter Limits from Pulse Shape Discrimination in a Low Background Sodium Iodide Detector at the Boulby Mine
 GARCIA 1995
PR D51 1458 Results of a Dark Matter Search with a Germanium Detector in the Canfranc Tunnel
 QUENBY 1995
PL B351 70 Results from the First Stage of a UK Galactic Dark Matter Search using Low Background Sodium Iodide Detectors
 SNOWDEN-IFFT 1995
PRL 74 4133 Limits on Dark Matter using Ancient Mica
 BECK 1994
PL B336 141 Searching for Dark Matter with the Enriched ${}^{}\mathrm {Ge}$ Detectors of the Heidelberg-Moscow Double $\beta$ Decay Experiment
 BACCI 1992
PL B293 460 WIMPs Search with Low Activity NaI Crystals. Preliminary Results
 REUSSER 1991
PL B255 143 Limits on Cold Dark Matter from the Gotthard ${}^{}\mathrm {Ge}$ Experiment
 CALDWELL 1988
PRL 61 510 Laboratory Limits on Galactic Cold Dark Matter