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

For ${\mathit m}_{{{\mathit X}^{0}}}$ = 100 GeV

INSPIRE JSON (beta) PDGID:

For limits from ${{\mathit X}^{0}}$ annihilation in the Sun, the assumed annihilation final state is shown in parenthesis in the comment.

S030DI2

VALUE (pb)

CL%

DOCUMENT ID

TECN

COMMENT

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

$<3 \times 10^{-12}$

90

LZ

SI wimp DM search

$<3.9 \times 10^{-11}$

90

XENT

wimp search

$<3 \times 10^{-11}$

90

PNDX

wimp search

$<1 \times 10^{5}$

95

NIT

directional nano-imaging DM search

$<8 \times 10^{-8}$

90

C100

wimp search

$<1 \times 10^{-3}$

90

COSN

WIMP search

$<2.5 \times 10^{-11}$

90

LZ

SI scatter on ${}^{}\mathrm {Xe}$

$<2 \times 10^{-8}$

90

XMAS

WIMP search

$<6 \times 10^{-11}$

90

XENT

SI WIMP search

$<6 \times 10^{-11}$

90

PNDX

${}^{}\mathrm {Xe}$ WIMP search

DEAP

${}^{}\mathrm {Ar}$

$<5 \times 10^{-5}$

SMPL

${}^{}\mathrm {W}$

$<4.2 \times 10^{-10}$

90

PNDX

${}^{}\mathrm {Xe}$ TPC

$<4 \times 10^{-8}$

90

XMAS

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

$<3.9 \times 10^{-9}$

90

DEAP

${}^{}\mathrm {Ar}$

$<2.3 \times 10^{-6}$

90

C100

${}^{}\mathrm {NaI}$

$<1.14 \times 10^{-8}$

90

DS50

${}^{}\mathrm {Ar}$

$<2 \times 10^{-8}$

90

CDMS

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

$<1.2 \times 10^{-8}$

90

DEAP

${}^{}\mathrm {Ar}$

$<9.12 \times 10^{-11}$

90

XE1T

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

PNDX

SIDM at PDX-II

$<1.7 \times 10^{-10}$

90

LUX

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

$<1.2 \times 10^{-10}$

90

XE1T

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

$<1.2 \times 10^{-10}$

90

PNDX

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

$<2.0 \times 10^{-8}$

90

DS50

${}^{}\mathrm {Ar}$

$<1 \times 10^{-9}$

90

LUX

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

$<1 \times 10^{-9}$

90

X100

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

$<2 \times 10^{-8}$

90

PNDX

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

$<4 \times 10^{-10}$

90

PNDX

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

$<6 \times 10^{-8}$

90

DS50

${}^{}\mathrm {Ar}$

$<4 \times 10^{-8}$

90

CDM2

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

$<7.13 \times 10^{-6}$

90

SKAM

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)

$<6.26 \times 10^{-7}$

90

SKAM

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit W}^{+}}{{\mathit W}^{-}}$)

$<2.76 \times 10^{-7}$

90

SKAM

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$)

$<1.5 \times 10^{-8}$

90

PNDX

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

$<1 \times 10^{-9}$

90

LUX

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

$<4.0 \times 10^{-6}$

90

BAIK

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit W}^{+}}{{\mathit W}^{-}}$)

$<1.0 \times 10^{-4}$

90

BAIK

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)

$<1.6 \times 10^{-6}$

90

BAIK

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$)

$<5 \times 10^{-6}$

90

SMPL

C$_{2}$ClF$_{5}$

$<6.01 \times 10^{-7}$

90

ICCB

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit W}^{+}}{{\mathit W}^{-}}$)

$<3.30 \times 10^{-5}$

90

ICCB

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)

$<1.9 \times 10^{-6}$

90

ADRIAN-MARTIN..

ANTR

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit W}^{+}}{{\mathit W}^{-}}$)

$<1.2 \times 10^{-4}$

90

ADRIAN-MARTIN..

ANTR

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)

$<7.6 \times 10^{-7}$

90

ADRIAN-MARTIN..

ANTR

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$)

$<2 \times 10^{-6}$

90

CDM2

${}^{}\mathrm {Si}$

$<1.6 \times 10^{-6}$

90

BAKS

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit W}^{+}}{{\mathit W}^{-}}$)

$<1.9 \times 10^{-5}$

90

BAKS

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)

$<7.1 \times 10^{-7}$

90

BAKS

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$)

$<3.2 \times 10^{-4}$

90

TEXO

WIMPs on ${}^{}\mathrm {Ge}$

$<1.67 \times 10^{-6}$

90

ICCB

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit W}^{+}}{{\mathit W}^{-}}$)

$<1.07 \times 10^{-4}$

90

ICCB

${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ (${{\mathit b}}{{\overline{\mathit b}}}$)

$<4 \times 10^{-8}$

90

ZEP3

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

$<1.4 \times 10^{-6}$

90

CRES

CaWO$_{4}$

$<3 \times 10^{-9}$

90

X100

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

$<3 \times 10^{-7}$

90

COUP

CF$_{3}$I

$<7 \times 10^{-6}$

SMPL

C$_{2}$ClF$_{5}$

$<2.5 \times 10^{-7}$

90

KIMS

CsI

$<2 \times 10^{-4}$

90

CGNT

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

CDM2

${}^{}\mathrm {Ge}$, inelastic

$<3.3 \times 10^{-8}$

90

RVUE

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

FLAT

$<3 \times 10^{-8}$

90

X100

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

X100

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

$<1 \times 10^{-8}$

90

X100

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

$<5 \times 10^{-8}$

90

EDE2

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

ZEP3

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

$<4 \times 10^{-8}$

90

CDM2

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

$<9 \times 10^{-6}$

90

CDM2

${}^{}\mathrm {Si}$, ${}^{}\mathrm {Ge}$, low threshold

ZEP3

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

$<5 \times 10^{-8}$

90

X100

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

$<1 \times 10^{-7}$

90

EDE2

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

$<3 \times 10^{-5}$

90

SMPL

C$_{2}$ClF$_{3}$

$<5 \times 10^{-8}$

90

CDM2

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

XE10

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

$<3 \times 10^{-4}$

90

TEXO

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

RVUE

¹	AALBERS 2025 search for WIMP DM using 4.2 ton-year LZ exposure. No signal observed. Limits placed in m(DM) vs. ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) plane.

²	APRILE 2025B search for wimps using 3.1 ton-years of data. No signal observed. Limits placed in ${{\mathit \sigma}^{SI}}$ vs m(${{\mathit \chi}}$) plane.

³	BO 2025 search for wimp dark matter with PandaX-4T. No signal detected. Limits placed in ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) vs. m(${{\mathit \chi}}$) plane.

⁴	UMEMOTO 2025 use directional DM search in nano-imaging tracking (NIT) emulsion device. No signal observed. Limits placed in ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) vs. m(${{\mathit \chi}}$) plane.

⁵	YU 2025 report on COSINE-100 wimp search in 3-year data. No signal observed. Limits placed in ${{\mathit \sigma}^{SI}}$ vs m(${{\mathit \chi}}$) plane.

⁶	ANGLOHER 2024A search for WIMP scatter on ${}^{}\mathrm {NaI}$ target. No signal observed. Limits placed in ${{\mathit \sigma}^{SI}}$ vs m plane.

⁷	AALBERS 2023 present first LZ limits on SI WIMP-nucleon scatter from ${}^{}\mathrm {Xe}$. ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit p}}$) $<$ $2.5 \times 10^{-11}$ pb for m(${{\mathit \chi}}$) = 100 GeV.

⁸	ABE 2023E search for WIMP scatter on ${}^{}\mathrm {Xe}$ in XMASS. No signal observed. Require ${{\mathit \sigma}^{SI}}$ $<$ $2 \times 10^{-7}$ pb for m(${{\mathit \chi}}$) = 100 GeV.

⁹	APRILE 2023A present first results from Xe-nton SI WIMP search. No signal observed. Quoted limit is for m(${{\mathit \chi}}$) = 100 GeV.

¹⁰	MENG 2021B search for SI WIMP interaction with 3.7 t ${}^{}\mathrm {Xe}$ and 0.63 t yr exposure. No signal observed. Limits placed in m(DM) vs. ${{\mathit \sigma}}{}^{SI}$ plane.

¹¹	ADHIKARI 2020 search for SI WIMP scatter from ${}^{}\mathrm {Ar}$ in AJAJ 2019 data. No signal observed. Limits placed on ${{\mathit \sigma}^{p}}$ vs. m(WIMP) for various assumed operators and models.

¹²	FELIZARDO 2020 presents 2014 SIMPLE bounds on WIMP DM using ${}^{}\mathrm {C}_{2}{}^{}\mathrm {Cl}{}^{}\mathrm {F}_{5}$ target.

¹³	WANG 2020G search for SI WIMP scatter on ${}^{}\mathrm {Xe}$ with 132 t d exposure of PANDAX-II.

¹⁴	ABE 2019 search for SI DD in single phase ${}^{}\mathrm {Xe}$; no signal; require ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit p}}$) $<$ $4 \times 10^{-8}$ pb for m(${{\mathit \chi}}$) $\sim{}$ 100 GeV.

¹⁵	AJAJ 2019 search for SI WIMP-nucleon scatter with 758 tonne day exposure of single phase liquid ${}^{}\mathrm {Ar}$; no signal: require ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) $<$ $3.9 \times 10^{-9}$ pb for m(${{\mathit \chi}}$) = 100 GeV.

¹⁶	ADHIKARI 2018 search for WIMP scatter on ${}^{}\mathrm {NaI}$;limit set ${{\mathit \sigma}}{}^{SI}({{\mathit \chi}}{{\mathit p}}$) $<$ $2.3 \times 10^{-6}$ pb for m(${{\mathit \chi}}$) = 100 GeV.

¹⁷	AGNES 2018A search for WIMP scatter on 46.4 kg ${}^{}\mathrm {Ar}$; no signal; require ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) $<$ $1.14 \times 10^{-8}$ pb for m(${{\mathit \chi}}$) = 100 GeV.

¹⁸	AGNESE 2018A set limit ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) $<$ $2 \times 10^{-8}$ pb for m(WIMP) = 100 GeV.

¹⁹	AMAUDRUZ 2018 search for WIMP scatter on ${}^{}\mathrm {Ar}$ with DEAP-3600; limits set: ${{\mathit \sigma}}{}^{SI}({{\mathit \chi}}$p) $<$ $1.2 \times 10^{-8}$ pb for m(WIMP) = 100 GeV.

²⁰	APRILE 2018 search for WIMP scatter on 1.3 t liquid ${}^{}\mathrm {Xe}$; no signal; require ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit p}}$) $<$ $9.12 \times 10^{-11}$ pb for m(${{\mathit \chi}}$) = 100 GeV.

²¹	REN 2018 search for self-interacting DM at Panda-X-II with a total exposure of 54 ton day; limits set in m(DM) vs. m(mediator) plane.

²²	AKERIB 2017 exclude SI cross section $>$ $1.7 \times 10^{-10}$ pb for m(WIMP) = 100 GeV. Uses complete LUX data set.

²³	APRILE 2017G set limit $\sigma {}^{SI}({{\mathit \chi}}{{\mathit p}}$) $<$ 1.2 $10^{-10}$ pb for m(WIMP) = 100 GeV using 1 ton fiducial mass ${}^{}\mathrm {Xe}$ TPC. Exposure is 34.2 live days.

²⁴	CUI 2017A search for SI WIMP scatter; limits placed in ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) vs. m(${{\mathit \chi}}$) plane for m $\sim{}$ $10 - 1 \times 10^{4}$ GeV using 54 ton-day exposure of ${}^{}\mathrm {Xe}$.

²⁵	AKERIB 2016 re-analysis of 2013 data exclude SI cross section $>$ $1 \times 10^{-9}$ pb for $\mathit m$(WIMP) = 100 GeV on ${}^{}\mathrm {Xe}$ target.

²⁶	APRILE 2016B combined 447 live days using ${}^{}\mathrm {Xe}$ target exclude ${{\mathit \sigma}}$(SI) $>$ $1.1 \times 10^{-9}$ pb for m(WIMP) = 50 GeV.

²⁷	TAN 2016 search for WIMP scatter off ${}^{}\mathrm {Xe}$ target; see SI exclusion plot Fig. 6.

²⁸	TAN 2016B search for WIMP-${{\mathit p}}$ scatter off ${}^{}\mathrm {Xe}$ target; see Fig. 5 for SI exclusion.

²⁹	AGNESE 2015B reanalyse AHMED 2010 data.

³⁰	XIAO 2015 search for WIMP scatter on ${}^{}\mathrm {Xe}$ with PandaX-I; limits placed in ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) vs. m(${{\mathit \chi}}$) plane for m(${{\mathit \chi}}$) $\sim{}$ $5 - 100$ GeV.

³¹	AVRORIN 2014 search for neutrinos from the Sun arising from the pair annihilation of ${{\mathit X}^{0}}$ trapped by the Sun in data taken between 1998 and 2003. See their Table 1 for limits assuming annihilation into neutrino pairs.

³²	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.

³³	ADRIAN-MARTINEZ 2013 search for neutrinos from the Sun arising from the pair annihilation of ${{\mathit X}^{0}}$ trapped by the sun in data taken between Jan. 2007 and Dec. 2008.

³⁴	AGNESE 2013 use data taken between Oct. 2006 and July 2007.

³⁵	BOLIEV 2013 search for neutrinos from the Sun arising from the pair annihilation of ${{\mathit X}^{0}}$ trapped by the sun in data taken from 1978 to 2009. See also SUVOROVA 2013 for an older analysis of the same data.

³⁶	LI 2013B search for WIMP scatter on ${}^{}\mathrm {Ge}$; limits placed in ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) vs. m(${{\mathit \chi}}$) plane for m(${{\mathit \chi}}$) $\sim{}$ $4 - 100$ GeV.

³⁷	ABBASI 2012 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.

³⁸	Reanalysis of ANGLOHER 2009 data with all three nuclides. See also BROWN 2012.

³⁹	See also APRILE 2014A.

⁴⁰	See their Fig. 6 for a limit on inelastically scattering ${{\mathit X}^{0}}$ for ${\mathit m}_{{{\mathit X}^{0}}}$ = 70 GeV.

⁴¹	AHMED 2011 search for ${{\mathit X}^{0}}$ inelastic scattering. See their Fig. $8 - 10$ for limits.

⁴²	AHMED 2011A combine CDMS and EDELWEISS data.

⁴³

AJELLO 2011 search for ${{\mathit e}^{\pm}}$ flux from ${{\mathit X}^{0}}$ annihilations in the Sun. Models in which ${{\mathit X}^{0}}$ annihilates into an intermediate long-lived weakly interacting particles or ${{\mathit X}^{0}}$ scatters inelastically are constrained. See their Fig. $6 - 8$ for limits.

⁴⁴	APRILE 2011 reanalyze APRILE 2010 data.

⁴⁵	APRILE 2011A search for ${{\mathit X}^{0}}$ inelastic scattering. See their Fig. 2 and 3 for limits. See also APRILE 2014A.

⁴⁶	Supersedes ARMENGAUD 2010. A limit on inelastic cross section is also given.

⁴⁷	HORN 2011 perform detector calibration by neutrons. Earlier results are only marginally affected.

⁴⁸	AKIMOV 2010 give cross section limits for inelastically scattering dark matter. See their Fig.$~$4.

⁴⁹	Superseded by AHMED 2010.

⁵⁰	ANGLE 2009 search for ${{\mathit X}^{0}}$ inelastic scattering. See their Fig. 4 for limits.

⁵¹	GIULIANI 2005 analyzes the spin-independent ${{\mathit X}^{0}}$-nucleon cross section limits with both isoscalar and isovector couplings. See their Fig. 3 and 4 for limits on the couplings.

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