χ~10−p elastic cross section

Experimental results on the χ~10−p elastic cross section are evaluated at mχ~10=100 GeV. The experimental results on the cross section are often mass dependent. Therefore, the mass and cross section results are also given where the limit is strongest, when appropriate. Results are quoted separately for spin-dependent interactions (based on an effective 4-Fermi Lagrangian of the form χ―γμγ5χq―γμγ5q) and spin-independent interactions (χ―χq―q). For calculational details see GRIEST 1988B, ELLIS 1988D, BARBIERI 1989C, DREES 1993B, ARNOWITT 1996, BERGSTROM 1996, and BAER 1997 in addition to the theory papers listed in the Tables. For a description of the theoretical assumptions and experimental techniques underlying most of the listed papers, see the review on “Dark matter” in this “Review of Particle Physics,” and references therein. Most of the following papers use galactic halo and nuclear interaction assumptions from (LEWIN 1996).

Spin-independent interactions

INSPIRE   PDGID:
S046DM2
VALUE (pb) CL% DOCUMENT ID TECN  COMMENT
• • We do not use the following data for averages, fits, limits, etc. • •
<3×10−11 90 1
AALBERS
2023
LZ Xe
<6.1×10−11 90 2
APRILE
2023A
 XENT Xe
<6.5×10−11 90 3
MENG
2021B
 PNDX Xe
<5×10−10 90 4
WANG
2020G
 PNDX Xe
<2.5×10−8 90 5
ABE
2019
XMAS Xe
<3.9×10−9 90 6
AJAJ
2019
DEAP Ar
<2×10−8 90 7
AMOLE
2019
PICO C3F8
<2.25×10−6 90 8
ADHIKARI
2018
C100 NaI
<1.14×10−8 90 9
AGNES
2018A
 DS50 Ar
<1.6×10−8 90 10
AGNESE
2018A
 CDMS Ge
<9×10−11 90 11
APRILE
2018
XE1T Xe
<1.8×10−10 90 12
AKERIB
2017
LUX Xe
<1.5×10−9 90 13
APRILE
2016B
 X100 Xe
<1.5×10−9 90 14
AKERIB
2014
LUX Xe
10−11−10−7 95 15
BUCHMUELLER
2014A
 THEO
<4.6×10−6 90 16
FELIZARDO
2014
SMPL C2ClF5
10−11−10−8 95 17
ROSZKOWSKI
2014
THEO
<2.2×10−6 90 18
AGNESE
2013
CDMS Si
<5×10−8 90 19
AKIMOV
2012
ZEP3 Xe
1.6×10−6;3.7×10−5 20
ANGLOHER
2012
CRES CaWO4
3×10−12 to 3 ×10−9 95 21
BECHTLE
2012
THEO
<1.6×10−7 22
BEHNKE
2012
COUP CF3I
<2.3×10−7 90 23
KIM
2012
KIMS CsI
<3.3×10−8 90 24
AHMED
2011A
 Ge
<4.4×10−8 90 25
ARMENGAUD
2011
EDE2 Ge
<1×10−7 90 26
ANGLE
2008
XE10 Xe
<1×10−6 90
BENETTI
2008
WARP Ar
<7.5×10−7 90 27
ALNER
2007A
 ZEP2 Xe
<2×10−7 28
AKERIB
2006A
 CDMS Ge
<90×10−7
ALNER
2005
NAIA NaI Spin Indep.
<12×10−7 29
ALNER
2005A
 ZEPL
<14×10−7
SANGLARD
2005
EDEL Ge
<4×10−7 30
AKERIB
2004
CDMS Ge
2×10−11 to 1.5 ×10−7 95 31
BALTZ
2004
THEO
2×10−11 to 8 ×10−6 32, 33
ELLIS
2004
THEO μ > 0
<5×10−8 34
PIERCE
2004A
 THEO
<2×10−5 35
AHMED
2003
NAIA NaI Spin Indep.
<3×10−6 36
AKERIB
2003
CDMS Ge
2×10−13 to 2 ×10−7 37
BAER
2003A
 THEO
<1.4×10−5 38
KLAPDOR-KLEIN..
2003
HDMS Ge
<6×10−6 39
ABRAMS
2002
CDMS Ge
1×10−12 to 7 ×10−6 32
KIM
2002B
 THEO
<3×10−5 40
MORALES
2002B
 CSME Ge
<1×10−5 41
MORALES
2002C
 IGEX Ge
<1×10−6
BALTZ
2001
THEO
<3×10−5 42
BAUDIS
2001
HDMS Ge
<7×10−6 43
BOTTINO
2001
THEO
<1×10−8 44
CORSETTI
2001
THEO tan β≤25
5×10−10 to 1.5 ×10−8 45
ELLIS
2001C
 THEO tan β≤10
<4×10−6 44
GOMEZ
2001
THEO
2×10−10 to 1 ×10−7 44
LAHANAS
2001
THEO
<3×10−6
ABUSAIDI
2000
CDMS Ge, Si
<6×10−7 46
ACCOMANDO
2000
THEO
47
BERNABEI
2000
DAMA NaI
2.5×10−9 to 3.5 ×10−8 48
FENG
2000
THEO tan β=10
<1.5×10−5
MORALES
2000
IGEX Ge
<4×10−5
SPOONER
2000
UKDM NaI
<7×10−6
BAUDIS
1999
HDMO 76Ge
<7×10−6
BERNABEI
1998C
 DAMA Xe
1  The strongest upper limit is 9.2×10−12 pb at 36 GeV.
2  The strongest upper limit is 2.6×10−11 pb at 28 GeV.
3  Commissioning Run for PandaX-4T. The strongest limit is 3.8×10−11 pb at mχ = 40 GeV.
4  WANG 2020G strongest limit is 2.2×10−10 pb at 30 GeV using 132 ton-day full exposure of PandaX-II. This updates CUI 2017A, though the results here provide weaker constraints.
5  The strongest upper limit is 2.2×10−8 pb at 60 GeV.
6  This updates AMAUDRUZ 2018.
7  This updates AMOLE 2016.
8  The strongest limit is 2.05×10−6 at m = 60 GeV.
9  The strongest limit is 1.09×10−8 pb at mχ = 126 GeV. This updates AGNES 2015.
10  The strongest limit is 1.0×10−8 pb at mχ = 46 GeV. This updates AGNESE 2015B.
11  Based on 278.8 days of data collection. The strongest limit is 4.1×10−11 pb at mχ = 30 GeV. This updates APRILE 2017G.
12  AKERIB 2017. The strongest limit is 1.1×10−10 pb at 50 GeV. This updates AKERIB 2016.
13  The strongest limit is 1.1×10−9 pb at 50 GeV. This updates APRILE 2012.
14  The strongest upper limit is 7.6×10−10 at mχ = 33 GeV.
15  Predictions for the spin-independent elastic cross section based on a frequentist approach to electroweak observables in the framework of N = 1 supergravity models with radiative breaking of the electroweak gauge symmetry using the 20 fb−1 8 TeV and the 5 fb−1 7 TeV LHC data and the LUX data.
16  The strongest limit is 3.6×10−6 pb and occurs at mχ = 35 GeV. Felizardo 2014 updates Felizardo 2012.
17  Predictions for the spin-independent elastic cross section based on a Bayesian approach to electroweak observables in the framework of N = 1 supergravity models with radiative breaking of the electroweak gauge symmetry using the 20 fb−1 LHC data and LUX.
18  AGNESE 2013 presents 90% CL limits on the elastic cross section for masses in the range 7−100 GeV using the Si based detector. The strongest upper limit is 1.8×10−6 pb at mχ = 50 GeV. This limit is improved to 7×10−7 pb in AGNESE 2013A.
19  This result updates LEBEDENKO 2009. The strongest limit is 3.9×10−8 pb at mχ = 52 GeV.
20  ANGLOHER 2012 presents results of 730 kg days from the CRESST-II dark matter detector. They find two maxima in the likelihood function corresponding to best fit WIMP masses of 25.3 and 11.6 GeV with elastic cross sections of 1.6×10−6 and 3.7×10−5 pb respectively, see their Table 4. The statistical significance is more than 4σ. ANGLOHER 2012 updates ANGLOHER 2009
21  Predictions for the spin-independent elastic cross section based on a frequentist approach to electroweak observables in the framework of N = 1 supergravity models with radiative breaking of the electroweak gauge symmetry using the 5 fb−1 LHC data and XENON100.
22  The strongest limit is 1.4×10−7 at mχ = 60 GeV.
23  This result updates LEE 2007A. The strongest limit is 2.1×10−7 at mχ = 70 GeV.
24  AHMED 2011A gives combined results from CDMS and EDELWEISS. The strongest limit is at mχ = 90 GeV.
25  ARMENGAUD 2011 updates result of ARMENGAUD 2010. Strongest limit at mχ = 85 GeV.
26  The strongest upper limit is 5.1×10−8 pb and occurs at mχ≃30 GeV. The values quoted here are based on the analysis performed in ANGLE 2008 with the update from SORENSEN 2009.
27  The strongest upper limit is 6.6×10−7 pb and occurs at mχ ≃ 65 GeV.
28  AKERIB 2006A updates the results of AKERIB 2005. The strongest upper limit is 1.6×10−7 pb and occurs at mχ ≈ 60 GeV.
29  The strongest upper limit is also close to 1.0×10−6 pb and occurs at mχ ≃ 70 GeV. BENOIT 2006 claim that the discrimination power of ZEPLIN-I measurement (ALNER 2005A) is not reliable enough to obtain a limit better than 1×10−3 pb. However, SMITH 2006 do not agree with the criticisms of BENOIT 2006.
30  AKERIB 2004 is incompatible with BERNABEI 2000 most likely value, under the assumption of standard WIMP-halo interactions. The strongest upper limit is 4×10−7 pb and occurs at mχ≃60 GeV.
31  Predictions for the spin-independent elastic cross section in the framework of N = 1 supergravity models with radiative breaking of the electroweak gauge symmetry.
32  KIM 2002 and ELLIS 2004 calculate the χp elastic scattering cross section in the framework of N=1 supergravity models with radiative breaking of the electroweak gauge symmetry, but without universal scalar masses.
33  In the case of universal squark and slepton masses, but non-universal Higgs masses, the limit becomes 2×10−6 (2×10−11 when constraint from the BNL g−2 experiment are included), see ELLIS 2003E. ELLIS 2005 display the sensitivity of the elastic scattering cross section to the π-Nucleon Σ term.
34  PIERCE 2004A calculates the χp elastic scattering cross section in the framework of models with very heavy scalar masses. See Fig. 2 of the paper.
35  The strongest upper limit is 1.8×10−5 pb and occurs at mχ≈80 GeV.
36  Under the assumption of standard WIMP-halo interactions, Akerib 03 is incompatible with BERNABEI 2000 most likely value at the 99.98% CL. See Fig. 4.
37  BAER 2003A calculates the χp elastic scattering cross section in several models including the framework of N=1 supergravity models with radiative breaking of the electroweak gauge symmetry.
38  The strongest upper limit is 7×10−6 pb and occurs at mχ≃30 GeV.
39  ABRAMS 2002 is incompatible with the DAMA most likely value at the 99.9% CL. The strongest upper limit is 3×10−6 pb and occurs at mχ≃30 GeV.
40  The strongest upper limit is 2×10−5 pb and occurs at mχ≃40 GeV.
41  The strongest upper limit is 7×10−6 pb and occurs at mχ≃46 GeV.
42  The strongest upper limit is 1.8×10−5 pb and occurs at mχ≃32 GeV
43  BOTTINO 2001 calculates the χ−p elastic scattering cross section in the framework of the following supersymmetric models: N=1 supergravity with the radiative breaking of the electroweak gauge symmetry, N=1 supergravity with nonuniversal scalar masses and an effective MSSM model at the electroweak scale.
44  Calculates the χ−p elastic scattering cross section in the framework of N=1 supergravity models with radiative breaking of the electroweak gauge symmetry.
45  ELLIS 2001C calculates the χ−p elastic scattering cross section in the framework of N=1 supergravity models with radiative breaking of the electroweak gauge symmetry. ELLIS 2002B find a range 2×10−8−1.5×10−7 at tan β=50. In models with nonuniversal Higgs masses, the upper limit to the cross section is 4×10−7.
46  ACCOMANDO 2000 calculate the χ−p elastic scattering cross section in the framework of minimal N=1 supergravity models with radiative breaking of the electroweak gauge symmetry. The limit is relaxed by at least an order of magnitude when models with nonuniversal scalar masses are considered. A subset of the authors in ARNOWITT 2002 updated the limit to <9×10−8 (tan β <55).
47  BERNABEI 2000 search for annual modulation of the WIMP signal. The data favor the hypothesis of annual modulation at 4σ and are consistent, for a particular model framework quoted there, with mX0=44 −9+12 GeV and a spin-independent X0-proton cross section of (5.4 ±1.0) ×10−6 pb. See also BERNABEI 2001 and BERNABEI 2000C.
48  FENG 2000 calculate the χ−p elastic scattering cross section in the framework of N=1 supergravity models with radiative breaking of the electroweak gauge symmetry with a particular emphasis on focus point models. At tan β=50, the range is 8×10−8−4×10−7.
References