Spin-Dependent Cross Section Limits for Dark Matter Particle (${{\mathit X}^{0}}$) on Proton

For ${\mathit m}_{{{\mathit X}^{0}}}$ = 20 GeV

INSPIRE   PDGID:
S030DP1
For limits from ${{\mathit X}^{0}}$ annihilation in the Sun, the assumed annihilation final state is shown in parenthesis in the comment.
VALUE (pb) CL% DOCUMENT ID TECN  COMMENT
• • We do not use the following data for averages, fits, limits, etc. • •
$<6 \times 10^{-5}$ 90 1
AALBERS
2023
LZ SD scatter on ${}^{}\mathrm {Xe}$
$<3.5 \times 10^{-5}$ 90 2
ABBASI
2022B
ICCB IceCube SD limit
$<1.5 \times 10^{5}$ 90 3
ANGLOHER
2022
CRES SD limit using ${}^{}\mathrm {Li}$
$<2 \times 10^{-4}$ 90 4
HUANG
2022
PNDX SD DM limits
$<9 \times 10^{-5}$ 90 5
AARTSEN
2020C
ICCB SD WIMP on ${{\mathit p}}$
$<2 \times 10^{5}$ 90 6
ABDELHAMEED
2020A
CRES ${}^{}\mathrm {LiAlO}_{2}$
$<5 \times 10^{-3}$ 7
FELIZARDO
2020
SMPL WIMPs via SIMPLE
$<3 \times 10^{5}$ 95 8
ABDELHAMEED
2019
CRES ${}^{7}\mathrm {Li}$
$<2.5 \times 10^{-5}$ 90 9
AMOLE
2019
PICO ${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$
$<2.5 \times 10^{-4}$ 90 10
APRILE
2019A
XE1T ${}^{}\mathrm {Xe}$, SD
$<1 \times 10^{-3}$ 90 11
XIA
2019A
PNDX SD WIMP on ${}^{}\mathrm {Xe}$
$<30$ 95 12
AGNESE
2018
SCDM ${}^{}\mathrm {Ge}$
$<1 \times 10^{-3}$ 90 13
AKERIB
2017A
LUX ${}^{}\mathrm {Xe}$
$<0.0132$ 90 14
BEHNKE
2017
PICA ${}^{}\mathrm {C}_{4}{}^{}\mathrm {F}_{10}$
$<2 \times 10^{-3}$ 90 15
FU
2017
PNDX SD WIMP on ${}^{}\mathrm {Xe}$
$<5 \times 10^{-4}$ 90 16
AMOLE
2016A
PICO ${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$
$<2 \times 10^{-6}$ 90 17
KHACHATRYAN
2016AJ
CMS 8 TeV ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit Z}}+\not E_T$; ${{\mathit Z}}$ $\rightarrow$ ${{\mathit \ell}}{{\overline{\mathit \ell}}}$
$<1.2 \times 10^{-3}$ 90
AMOLE
2015
PICO ${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$
$<1.43 \times 10^{-3}$ 90
CHOI
2015
SKAM ${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)
$<1.42 \times 10^{-4}$ 90
CHOI
2015
SKAM ${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$)
$<5 \times 10^{-3}$ 90
FELIZARDO
2014
SMPL C$_{2}$ClF$_{5}$
$<0.0129$ 90 18
AARTSEN
2013
ICCB ${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$)
$<0.0317$ 90 19
APRILE
2013
X100 ${}^{}\mathrm {Xe}$
$<0.03$ 90 20
ARCHAMBAULT
2012
PICA ${}^{}\mathrm {F}$ (C$_{4}F_{10}$)
$<0.06$ 90
BEHNKE
2012
COUP CF$_{3}$I
$<20$ 90
DAW
2012
DRFT F (CF$_{4}$)
$<7 \times 10^{-3}$
FELIZARDO
2012
SMPL C$_{2}$ClF$_{5}$
$<0.15$ 90
KIM
2012
KIMS CsI
$<1 \times 10^{5}$ 90 21
AHLEN
2011
DMTP F (CF$_{4}$)
$<0.1$ 90 21
BEHNKE
2011
COUP CF$_{3}$I
$<0.015$ 90 22
TANAKA
2011
SKAM ${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)
$<0.2$ 90
ARCHAMBAULT
2009
PICA ${}^{}\mathrm {F}$
$<4$ 90
LEBEDENKO
2009A
ZEP3 ${}^{}\mathrm {Xe}$
$<0.6$ 90
ANGLE
2008A
XE10 ${}^{}\mathrm {Xe}$
$<100$ 90
ALNER
2007
ZEP2 ${}^{}\mathrm {Xe}$
$<1$ 90
LEE
2007A
KIMS CsI
$<20$ 90 23
AKERIB
2006
CDMS ${}^{73}\mathrm {Ge}$, ${}^{29}\mathrm {Si}$
$<2$ 90
SHIMIZU
2006A
CNTR F (CaF$_{2}$)
$<0.5$ 90
ALNER
2005
NAIA NaI
$<1.5$ 90
BARNABE-HEIDE..
2005
PICA F (C$_{4}F_{10}$)
$<1.5$ 90
GIRARD
2005
SMPL F (C$_{2}$ClF$_{5}$)
$<35$ 90
MIUCHI
2003
BOLO LiF
$<30$ 90
TAKEDA
2003
BOLO NaF
1  AALBERS 2023 yield first SD LZ limits on WIMP-${{\mathit p}}$ scatter using ${}^{}\mathrm {Xe}$. ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ $6 \times 10^{-5}$ pb for m(${{\mathit \chi}}$) = 20 GeV.
2  ABBASI 2022B search for WIMP annihilation to ${{\mathit b}}{{\overline{\mathit b}}}$, ${{\mathit \tau}}{{\overline{\mathit \tau}}}$, ${{\mathit \nu}}{{\overline{\mathit \nu}}}$ in Sun with 7 years data; no signal; limits set in m(${{\mathit \chi}}$) vs. ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) plane for m(${{\mathit \chi}}$): $10 - 100$ GeV; quoted limit for ${{\mathit \nu}}{{\overline{\mathit \nu}}}$ channel.
3  ANGLOHER 2022 search for SD WIMP-proton scatter from ${}^{}\mathrm {Li}$ target; no signal detected; limits placed in ${{\mathit \sigma}}$ vs. m(WIMP) plane.
4  HUANG 2022 search for SD DM scatter on ${}^{}\mathrm {Xe}$; no signal observed; limits placed in ${\mathit \sigma (}{{\mathit \chi}}{{\mathit n}}{)}$ vs. m(DM) plane; quoted limit is for m(DM) = 20 GeV.
5  AARTSEN 2020C place combined IceCube and Pico-60 velocity-independent limits on spin-dependent WIMP-${{\mathit p}}$ scatter ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}})<$ $9 - 5$ pb for m(WIMP) = 20 GeV assuming dominant annihilation to ${{\mathit \tau}}{{\overline{\mathit \tau}}}$.
6  ABDELHAMEED 2020A use ${}^{}\mathrm {LiAlO}_{2}$ target in CRESST to search for spin-dependent WIMP scatter on ${{\mathit p}}$; limits set for m(WIMP): $0.3 - 30$ GeV in Fig. 8. Quoted limit is for M(WIMP) = 30 GeV.
7  FELIZARDO 2020 presents 2014 SIMPLE bounds on WIMP DM using ${}^{}\mathrm {C}_{2}{}^{}\mathrm {Cl}{}^{}\mathrm {F}_{5}$ target .
8  ABDELHAMEED 2019 uses ${}^{}\mathrm {Li}_{2}{}^{}\mathrm {MoO}_{4}$ target to set limit for spin dependent coupling ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ $3. \times 10^{5}$ pb for m(${{\mathit \chi}}$) = 20 GeV.
9  AMOLE 2019 search for SD WIMP scatter on ${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$ in PICO-60 bubble chamber; no signal: set limit for spin dependent coupling ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ $2.5 \times 10^{-5}$ pb for m(${{\mathit \chi}}$) = 20 GeV.
10  APRILE 2019A search for SD WIMP scatter on 1 t yr ${}^{}\mathrm {Xe}$; no signal, limits placed in ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) vs. m(${{\mathit \chi}}$) plane for m $\sim{}$ $6 - 1000$ GeV.
11  XIA 2019A search for WIMP scatter on ${}^{}\mathrm {Xe}$ in PandaX-II; limits placed in ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) vs. m(${{\mathit \chi}}$) plane for m(${{\mathit \chi}}$) $\sim{}$ $5 - 1 \times 10^{5}$ GeV.
12  AGNESE 2018 give limits for ${{\mathit \sigma}^{SD}}({{\mathit p}}{{\mathit \chi}}$) for m(WIMP) between 1.5 and 20 GeV using CDMSlite mode data.
13  AKERIB 2017A search for SD WIMP scatter on ${}^{}\mathrm {Xe}$ using 129.5 kg yr exposure; limits placed in ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) vs. m(${{\mathit \chi}}$) plane for m(${{\mathit \chi}}$) $\sim{}$ $6 - 1 \times 10^{5}$ GeV.
14  BEHNKE 2017 show final Picasso results based on 231.4 kg d exposure at SNOLab for WIMP scatter on ${}^{}\mathrm {C}_{4}{}^{}\mathrm {F}_{10}$ search via superheated droplet; require ${{\mathit \sigma}}$(SD) $<$ $1.32 \times 10^{-2}$ pb for m(WIMP) = 20 GeV.
15  FU 2017 search for SD WIMP scatter on ${}^{}\mathrm {Xe}$; limits set in ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) vs. m(${{\mathit \chi}}$) plane for m(${{\mathit \chi}}$) $\sim{}$ $4 - 1 \times 10^{3}$ GeV.
16  AMOLE 2016A require SD WIMP-${{\mathit p}}$ scattering $<$ $5 \times 10^{-4}$ pb for $\mathit m$(WIMP) = 20 GeV; bubbles from ${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$ target.
17  KHACHATRYAN 2016AJ require SD WIMP-${{\mathit p}}$ $<$ $2 \times 10^{-6}$ pb for $\mathit m$(WIMP) = 20 GeV from ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit Z}}$ + $\not E_T$; ${{\mathit Z}}$ $\rightarrow$ ${{\mathit \ell}}{{\overline{\mathit \ell}}}$ signal.
18  AARTSEN 2013 search for neutrinos from the Sun arising from the pair annihilation of ${{\mathit X}^{0}}$ trapped by the sun in data taken between June 2010 and May 2011.
19  The value has been provided by the authors. APRILE 2013 note that the proton limits on ${}^{}\mathrm {Xe}$ are highly sensitive to the theoretical model used. See also APRILE 2014A.
20  ARCHAMBAULT 2012 search for WIMP scatter on ${}^{}\mathrm {C}_{4}{}^{}\mathrm {F}_{10}$; limits set in ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) vs. m(${{\mathit \chi}}$) plane for m $\sim{}$ $4 - 500$ GeV.
21  Use a direction-sensitive detector.
22  TANAKA 2011 search for neutrinos from the Sun arising from the pair annihilation of ${{\mathit X}^{0}}$ trapped by the Sun. The amount of ${{\mathit X}^{0}}$ depends on the ${{\mathit X}^{0}}$-proton cross section.
23  See also AKERIB 2005.
References