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

For ${\boldsymbol m}_{{{\boldsymbol X}^{0}}}$ = 100 GeV INSPIRE search

VALUE (nb) CL% DOCUMENT ID TECN  COMMENT
• • • We do not use the following data for averages, fits, limits, etc. • • •
$<3 \times 10^{-3}$ 90 1
UCHIDA
2014
XMAS ${}^{129}\mathrm {Xe}$, inelastic
$<0.3$ 90 2
ANGLOHER
2002
CRES ${}^{}\mathrm {Al}$
3
BELLI
2002
RVUE
4
BERNABEI
2002C
DAMA
5
GREEN
2002
RVUE
6
ULLIO
2001
RVUE
7
BENOIT
2000
EDEL Ge
$<4 \times 10^{-3}$ 90 8
BERNABEI
2000D
${}^{129}\mathrm {Xe}$, inel.
9
AMBROSIO
1999
MCRO
10
BRHLIK
1999
RVUE
$<8 \times 10^{-3}$ 95 11
KLIMENKO
1998
CNTR ${}^{73}\mathrm {Ge}$, inel.
$<0.08$ 95 12
KLIMENKO
1998
CNTR ${}^{73}\mathrm {Ge}$, inel.
$<4$
ALESSANDRELLO
1996
CNTR ${}^{}\mathrm {O}$
$<25$
ALESSANDRELLO
1996
CNTR ${}^{}\mathrm {Te}$
$<6 \times 10^{-3}$ 90 13
BELLI
1996
CNTR ${}^{129}\mathrm {Xe}$, inel.
14
BELLI
1996C
CNTR ${}^{129}\mathrm {Xe}$
$<1 \times 10^{-3}$ 90 15
BERNABEI
1996
CNTR ${}^{}\mathrm {Na}$
$<0.3$ 90 15
BERNABEI
1996
CNTR ${}^{}\mathrm {I}$
$<0.7$ 95 16
SARSA
1996
CNTR ${}^{}\mathrm {Na}$
$<0.03$ 90 17
SMITH
1996
CNTR ${}^{}\mathrm {Na}$
$<0.8$ 90 17
SMITH
1996
CNTR ${}^{}\mathrm {I}$
$<0.35$ 95 18
GARCIA
1995
CNTR Natural ${}^{}\mathrm {Ge}$
$<0.6$ 95
QUENBY
1995
CNTR ${}^{}\mathrm {Na}$
$<3$ 95
QUENBY
1995
CNTR ${}^{}\mathrm {I}$
$<150$ 90 19
SNOWDEN-IFFT
1995
MICA ${}^{16}\mathrm {O}$
$<400$ 90 19
SNOWDEN-IFFT
1995
MICA ${}^{39}\mathrm {K}$
$<0.08$ 90 20
BECK
1994
CNTR ${}^{76}\mathrm {Ge}$
$<2.5$ 90
BACCI
1992
CNTR ${}^{}\mathrm {Na}$
$<3$ 90
BACCI
1992
CNTR ${}^{}\mathrm {I}$
$<0.9$ 90 21
REUSSER
1991
CNTR Natural ${}^{}\mathrm {Ge}$
$<0.7$ 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  BELLI 2002 discuss dependence of the extracted WIMP cross section on the assumptions of the galactic halo structure.
4  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 .
5  GREEN 2002 discusses dependence of extracted WIMP cross section limits on the assumptions of the galactic halo structure.
6  ULLIO 2001 disfavor the possibility that the BERNABEI 1999 signal is due to spin-dependent WIMP coupling.
7  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.
8  BERNABEI 2000D limit is for inelastic scattering ${{\mathit X}^{0}}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{129}\mathrm {Xe}$ (39.58 keV).
9  AMBROSIO 1999 search for upgoing muon events induced by neutrinos originating from WIMP annihilations in the Sun and Earth.
10  BRHLIK 1999 discuss the effect of astrophysical uncertainties on the WIMP interpretation of the BERNABEI 1999 signal.
11  KLIMENKO 1998 limit is for inelastic scattering ${{\mathit X}^{0}}$ $~{}^{73}\mathrm {Ge}$ $\rightarrow$ ${{\mathit X}^{0}}$ ${}^{73}\mathrm {Ge}{}^{*}$ ($13.26$ keV).
12  KLIMENKO 1998 limit is for inelastic scattering ${{\mathit X}^{0}}$ $~{}^{73}\mathrm {Ge}$ $\rightarrow$ ${{\mathit X}^{0}}$ ${}^{73}\mathrm {Ge}{}^{*}$ ($66.73$ keV).
13  BELLI 1996 limit for inelastic scattering ${{\mathit X}^{0}}$ ${}^{129}\mathrm {Xe}$ $\rightarrow$ ${{\mathit X}^{0}}{}^{129}\mathrm {Xe}^{*}(39.58$ keV).
14  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.
15  BERNABEI 1996 use pulse shape discrimination to enhance the possible signal. The limit here is from R.$~$Bernabei, private communication, September 19, 1997.
16  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.
17  SMITH 1996 use pulse shape discrimination to enhance the possible signal. A dark matter density of $0.4~$GeV$~$cm${}^{-3}$ is assumed.
18  GARCIA 1995 limit is from the event rate. A weaker limit is obtained from searches for diurnal and annual modulation.
19  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.
20  BECK 1994 uses enriched ${}^{76}\mathrm {Ge}$ (86$\%$ purity).
21  REUSSER 1991 limit here is changed from published ($0.3$) 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
BELLI 2002
PR D66 043503 Effect of the Galactic Halo Modeling on the DAMA/NaI Annual Modulation Result: an Extended Analysis of the Data for WIMPs with a Purely Spin Independent Coupling
BERNABEI 2002C
EPJ C23 61 Investigating the DAMA Annual Modulation Data in the Framework of Inelastic Dark Matter
GREEN 2002
PR D66 083003 Effect of Halo Modelling on WIMP Exclusion Limits
ULLIO 2001
JHEP 0107 044 Spin Dependent WIMPs in DAMA?
BENOIT 2000
PL B479 8 Event Categories in the EDELWEISS WIMP Search Experiment
BERNABEI 2000D
NJP 2 15 Improved Limits on WIMP ${}^{129}\mathrm {Xe}$ Inelastic Scattering
AMBROSIO 1999
PR D60 082002 Limits on Dark Matter WIMPs using Upward Going Muons in the MACRO Detector
BRHLIK 1999
PL B464 303 WIMP Velocity Impact on Direct Dark Matter Searches
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 1996C
NC C19 537 Search for WIMPs with Enriched Xenon at Gran Sasso
BELLI 1996
PL B387 222 Limits on WIMP $−$ ${}^{129}\mathrm {Xe}$ Inelastic Scattering
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
BERNABEI 1999
PL B450 448 On a Further Search for a Yearly Modulation of the Rate in Particle Dark Matter Direct Search
SMITH 2001
PR D64 043502 Inelastic Dark Matter