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

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. • •

$<1.5 \times 10^{-3}$

90

LZ

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

$<0.2$

90

C100

SD WIMP scatter on ${}^{}\mathrm {I}$

$<1.2 \times 10^{-3}$

90

PNDX

SD DM limits

$<200$

90

NAGE

directional gas TPC

$<4.81 \times 10^{-3}$

90

ICCB

SD WIMP on ${{\mathit p}}$

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

90

PICO

${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$

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

90

XE1T

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

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

90

PNDX

SD WIMP on ${}^{}\mathrm {Xe}$

HAWC

DM annihilation in Sun to long-lived mediator

$<2.05 \times 10^{-5}$

90

ICCB

${{\mathit \nu}}$, sun

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

90

LUX

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

$<0.02$

90

PNDX

SD WIMP on ${}^{}\mathrm {Xe}$

ADRIAN-MARTIN..

ANTR

solar ${{\mathit \mu}}$ from WIMP annih.

$<0.01$

90

PICO

${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$

$<1.5 \times 10^{3}$

90

NAGE

${}^{}\mathrm {C}{}^{}\mathrm {F}_{4}$

$<2.7 \times 10^{-3}$

90

BAIK

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

$<0.069$

90

BAIK

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

$<8.4 \times 10^{-4}$

90

BAIK

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

$<4.48 \times 10^{-4}$

90

ICCB

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

$<0.01$

90

ICCB

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

$<8.9 \times 10^{-4}$

90

ADRIAN-MARTIN..

ANTR

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

$<0.02$

90

ADRIAN-MARTIN..

ANTR

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

$<2.3 \times 10^{-4}$

90

ADRIAN-MARTIN..

ANTR

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

$<0.0757$

90

X100

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

$<5.4 \times 10^{-3}$

90

BAKS

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

$<0.042$

90

BAKS

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

$<1.5 \times 10^{-3}$

90

BAKS

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

$<2.50 \times 10^{-4}$

90

ICCB

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

$<7.86 \times 10^{-3}$

90

ICCB

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

$<0.08$

90

COUP

CF$_{3}$I

$<8$

90

DRFT

F (CF$_{4}$)

$<0.06$

SMPL

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

$<0.08$

90

KIMS

CsI

$<8 \times 10^{3}$

90

DMTP

F (CF$_{4}$)

$<0.4$

90

COUP

CF$_{3}$I

$<2 \times 10^{-3}$

90

SKAM

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

$<0.02$

90

SKAM

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

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

90

ICCB

KK dark matter

$<2 \times 10^{4}$

90

NAGE

CF$_{4}$

$<8.7 \times 10^{-4}$

90

ICCB

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

$<0.022$

90

ICCB

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

$<3$

90

PICA

${}^{}\mathrm {F}$

$<6$

90

ZEP3

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

$<9$

90

XE10

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

$<100$

90

ZEP2

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

$<0.8$

90

KIMS

CsI

$<4 \times 10^{4}$

90

NAGE

F (CF$_{4}$)

$<30$

90

CDMS

${}^{73}\mathrm {Ge}$, ${}^{29}\mathrm {Si}$

$<1.5$

90

NAIA

NaI

$<15$

90

BARNABE-HEIDE..

PICA

F (C$_{4}F_{10}$)

$<600$

90

EDEL

${}^{73}\mathrm {Ge}$

$<10$

90

SMPL

F (C$_{2}$ClF$_{5}$)

$<260$

90

BOLO

LiF

$<150$

90

BOLO

NaF

¹	AALBERS 2023 yield first SD LZ limits on WIMP-${{\mathit p}}$ scatter using ${}^{}\mathrm {Xe}$. ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ $2 \times 10^{-3}$ pb for m(${{\mathit \chi}}$) = 1 TeV.

²	ADHIKARI 2023C search for SD WIMP scatter on ${}^{}\mathrm {I}$. No signal observed. Require ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ 0.2 pb for m(${{\mathit \chi}}$) = 1 TeV.

³	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) = 1 TeV.

⁴	IKEDA 2021 use direction sensitive TPC NEWAGE to search for SD WIMPs. No signal observed. Limits set in ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) vs. m plane; ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ 200 pb for m(DM) = 1000 GeV.

⁵	AARTSEN 2020C place combined IceCube and Pico-60 velocity-independent limits on spin-dependent WIMP-${{\mathit p}}$ scatter ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ $3 \times 10^{-3}$ pb for m(WIMP) = 1 TeV assuming dominant annihilation to ${{\mathit W}}{{\mathit W}}$.

⁶	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 ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ $3 \times 10^{-4}$ pb for m(${{\mathit \chi}}$) = 1000 GeV.

⁷	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.

⁸	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.

⁹	ALBERT 2018C search for DM annihilation in Sun to long-lived mediator (LLM) which decays outside Sun, for DM masses above 1 TeV; assuming LLM, limits set on ${{\mathit \sigma}}{}^{SD}({{\mathit \chi}}{{\mathit p}}$).

¹⁰	AARTSEN 2017A search for neutrinos from solar WIMP annihilation into ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ in 532 days of live time.

¹¹	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.

¹²	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.

¹³	ADRIAN-MARTINEZ 2016B search for secluded DM via WIMP annihilation in solar core into light mediator which later decays to ${{\mathit \mu}}$ or ${{\mathit \nu}}$s; limits presented in Figures 3 and 4.

¹⁴	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.

¹⁵	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.

¹⁶	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.

¹⁷	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.

¹⁸	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.

¹⁹	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.

²⁰	Use a direction-sensitive detector.

²¹	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.

²²	ABBASI 2010 search for ${{\mathit \nu}_{{{\mu}}}}$ from annihilations of Kaluza-Klein photon dark matter in the Sun.

²³	See also AKERIB 2005.

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