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

For ${\mathit m}_{{{\mathit X}^{0}}}$ = 1 TeV

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. • •

$<2.8 \times 10^{-10}$

90

LZ

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

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

90

XMAS

WIMP search

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

90

PNDX

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

DEAP

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

$<4 \times 10^{-9}$

90

PNDX

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

$<3 \times 10^{-6}$

90

${}^{}\mathrm {Ar}$; I-spin viol DM

$<3.8 \times 10^{-8}$

90

DS50

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

$<8.24 \times 10^{-10}$

90

XE1T

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

$<2 \times 10^{-9}$

90

LUX

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

$<0.3$

90

PNDX

${{\mathit \chi}}$ ${{\mathit N}}$ $\rightarrow$ ${{\mathit \chi}^{*}}$ $\rightarrow$ ${{\mathit \chi}}{{\mathit \gamma}}$

$<1.2 \times 10^{-9}$

90

PNDX

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

$<8.6 \times 10^{-8}$

90

DS50

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

$<2 \times 10^{-7}$

90

DS50

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

$<2 \times 10^{-7}$

90

CDM2

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

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

90

LUX

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

$<2.2 \times 10^{-6}$

90

BAIK

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

$<5.5 \times 10^{-5}$

90

BAIK

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

$<6.8 \times 10^{-7}$

90

BAIK

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

$<3.46 \times 10^{-7}$

90

ICCB

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

$<7.75 \times 10^{-6}$

90

ICCB

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

$<6.9 \times 10^{-7}$

90

ADRIAN-MARTIN..

ANTR

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

$<1.5 \times 10^{-5}$

90

ADRIAN-MARTIN..

ANTR

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

$<1.8 \times 10^{-7}$

90

ADRIAN-MARTIN..

ANTR

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

$<4.3 \times 10^{-6}$

90

BAKS

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

$<3.4 \times 10^{-5}$

90

BAKS

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

$<1.2 \times 10^{-6}$

90

BAKS

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

$<2.12 \times 10^{-7}$

90

ICCB

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

$<6.56 \times 10^{-6}$

90

ICCB

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

$<4 \times 10^{-7}$

90

ZEP3

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

$<1.1 \times 10^{-5}$

90

CRES

CaWO$_{4}$

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

90

X100

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

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

90

COUP

CF$_{3}$I

$<4 \times 10^{-6}$

SMPL

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

$<1.5 \times 10^{-6}$

90

KIMS

CsI

CDM2

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

$<1.5 \times 10^{-7}$

90

RVUE

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

$<2 \times 10^{-7}$

90

X100

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

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

90

X100

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

$<2 \times 10^{-7}$

90

EDE2

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

ZEP3

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

$<2 \times 10^{-7}$

90

CDM2

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

$<4 \times 10^{-7}$

90

X100

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

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

90

EDE2

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

$<3.5 \times 10^{-7}$

90

CDM2

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

¹	AALBERS 2023 give first LZ limits on WIMP-nucleon scatter from ${}^{}\mathrm {Xe}$. ${{\mathit \sigma}^{SI}}$ $<$ $2.8 \times 10^{-10}$ pb for m(${{\mathit \chi}}$) = 1 TeV.

²	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(${{\mathit \chi}}$) = 1000 GeV.

³	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.

⁴	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.

⁵	WANG 2020G search for SI WIMP scatter on ${}^{}\mathrm {Xe}$ with 132 t d exposure of PANDAX-II .

⁶	YAGUNA 2019 recasts DEAP-3600 single-phase liquid argon results in limit for isospin violating DM; for ${{\mathit f}_{{{n}}}}/{{\mathit f}_{{{p}}}}$ = $-0.69$, requires ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit p}}$) $<$ $3 \times 10^{-6}$ pb for m(${{\mathit \chi}}$) = 1 TeV.

⁷	AGNES 2018A search for WIMP scatter on 46.4 kg ${}^{}\mathrm {Ar}$; no signal; require ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) $<$ $3.8 \times 10^{-8}$ pb for m(${{\mathit \chi}}$) = 1 TeV.

⁸	APRILE 2018 search for WIMP scatter on 1.3 t ${}^{}\mathrm {Xe}$; no signal seen; require ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit p}}$) $<$ $8.24 \times 10^{-10}$ pb for m(${{\mathit \chi}}$) = 1 TeV.

⁹	AKERIB 2017 search for WIMP scatter on ${}^{}\mathrm {Xe}$ using complete LUX data set; limits placed in ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) vs. m(${{\mathit \chi}}$) plane for m(${{\mathit \chi}}$) $\sim{}$ $5 - 1 \times 10^{5}$ GeV.

¹⁰	CHEN 2017E search for inelastic WIMP scatter on ${}^{}\mathrm {Xe}$; require ${{\mathit \sigma}}{}^{SI}({{\mathit \chi}}{{\mathit N}}$) $<$ 0.3 pb for m(${{\mathit \chi}}$) = 1 TeV and (mass difference) = 300 keV.

¹¹	CUI 2017A search for WIMP scatter using 54 ton-day exposure of ${}^{}\mathrm {Xe}$; limits placed in ${{\mathit \sigma}^{SI}}({{\mathit \chi}}{{\mathit N}}$) vs. m(${{\mathit \chi}}$) plane for m $\sim{}$ $10 - 1 \times 10^{4}$ GeV.

¹²	AGNESE 2015B reanalyse AHMED 2010 data.

¹³	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.

¹⁴	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.

¹⁵	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.

¹⁶	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.

¹⁷	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.

¹⁸	Reanalysis of ANGLOHER 2009 data with all three nuclides. See also BROWN 2012.

¹⁹	See also APRILE 2014A.

²⁰	AHMED 2011 search for ${{\mathit X}^{0}}$ inelastic scattering. See their Fig. $8 - 10$ for limits.

²¹	AHMED 2011A combine CDMS and EDELWEISS data.

²²	APRILE 2011 reanalyze APRILE 2010 data.

²³	Supersedes ARMENGAUD 2010. A limit on inelastic cross section is also given.

²⁴	HORN 2011 perform detector calibration by neutrons. Earlier results are only marginally affected.

²⁵	Superseded by AHMED 2010.

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