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

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

VALUE (pb)

CL%

DOCUMENT ID

TECN

COMMENT

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

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

90

LZ

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

$<3.5 \times 10^{-5}$

90

ICCB

IceCube SD limit

$<1.5 \times 10^{5}$

90

CRES

SD limit using ${}^{}\mathrm {Li}$

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

90

PNDX

SD DM limits

$<9 \times 10^{-5}$

90

ICCB

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

$<2 \times 10^{5}$

90

CRES

${}^{}\mathrm {LiAlO}_{2}$

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

SMPL

WIMPs via SIMPLE

$<3 \times 10^{5}$

95

CRES

${}^{7}\mathrm {Li}$

$<2.5 \times 10^{-5}$

90

PICO

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

$<2.5 \times 10^{-4}$

90

XE1T

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

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

90

PNDX

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

$<30$

95

SCDM

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

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

90

LUX

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

$<0.0132$

90

PICA

${}^{}\mathrm {C}_{4}{}^{}\mathrm {F}_{10}$

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

90

PNDX

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

$<5 \times 10^{-4}$

90

PICO

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

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

90

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

PICO

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

$<1.43 \times 10^{-3}$

90

SKAM

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

$<1.42 \times 10^{-4}$

90

SKAM

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

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

90

SMPL

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

$<0.0129$

90

ICCB

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

$<0.0317$

90

X100

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

$<0.03$

90

PICA

${}^{}\mathrm {F}$ (C$_{4}F_{10}$)

$<0.06$

90

COUP

CF$_{3}$I

$<20$

90

DRFT

F (CF$_{4}$)

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

SMPL

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

$<0.15$

90

KIMS

CsI

$<1 \times 10^{5}$

90

DMTP

F (CF$_{4}$)

$<0.1$

90

COUP

CF$_{3}$I

$<0.015$

90

SKAM

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

$<0.2$

90

PICA

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

$<4$

90

ZEP3

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

$<0.6$

90

XE10

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

$<100$

90

ZEP2

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

$<1$

90

KIMS

CsI

$<20$

90

CDMS

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

$<2$

90

CNTR

F (CaF$_{2}$)

$<0.5$

90

NAIA

NaI

$<1.5$

90

BARNABE-HEIDE..

PICA

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

$<1.5$

90

SMPL

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

$<35$

90

BOLO

LiF

$<30$

90

BOLO

NaF

¹	AALBERS 2023 yield first SD LZ limits on WIMP-${{\mathit p}}$ scatter using ${}^{}\mathrm {Xe}$. ${{\mathit \sigma}^{SD}}({{\mathit \chi}}{{\mathit p}}$) $<$ $6 \times 10^{-5}$ 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.

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