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

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. • •
$<5 \times 10^{-11}$ 90 1
 2021 B
PNDX ${}^{}\mathrm {Xe}$ WIMP search
$<5 \times 10^{-5}$ 2
 2020
SMPL ${}^{}\mathrm {C}_{2}{}^{}\mathrm {Cl}{}^{}\mathrm {F}_{5}$
$<2.2 \times 10^{-10}$ 90 3
 2020 G
PNDX ${}^{}\mathrm {Xe}$ TPC
4
 2019
CRES ${}^{}\mathrm {Ca}{}^{}\mathrm {W}{}^{}\mathrm {O}_{4}$
$<7 \times 10^{-5}$ 90 5
 2019 A
KIMS ${}^{}\mathrm {NaI}$
$<3 \times 10^{-7}$ 90 6
 2019
XMAS SI WIMP on ${}^{}\mathrm {Xe}$
7
 2019
BELL ${{\mathit \Upsilon}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit A}}$ , ${{\mathit A}}$ $\rightarrow$ ${{\mathit \chi}}{{\mathit \chi}}$
$<3.5 \times 10^{-5}$ 90 8
 2019
CDEX annual modulation ${}^{}\mathrm {Ge}$
$<2 \times 10^{-7}$ 90 9
 2018 C
XMAS ${{\mathit X}^{0}} - {}^{}\mathrm {Xe}$ modulation
$<1.44 \times 10^{-5}$ 90 10
 2018
C100 ${}^{}\mathrm {NaI}$
$<3 \times 10^{-7}$ 90 11
 2018
DS50 ${{\mathit X}^{0}}$ -${}^{}\mathrm {Ar}$
$<5 \times 10^{-6}$ 95 12
 2018
SCDM ${}^{}\mathrm {Ge}$
$<4 \times 10^{-8}$ 90 13
 2018 A
SCDM ${}^{}\mathrm {Ge}$
$<6 \times 10^{-11}$ 90 14
 2018
XE1T ${}^{}\mathrm {Xe}$, SI
$<4.5 \times 10^{-3}$ 90 15
 2018
NEWS GeV WIMPs on ${}^{}\mathrm {Ne}$
$<2 \times 10^{-6}$ 90 16
 2017
ICCB ${{\mathit \nu}}$ , earth
$<2 \times 10^{-10}$ 90 17
 2017
LUX ${}^{}\mathrm {Xe}$
$<1 \times 10^{-3}$ 90 18
 2017
ICCB ${}^{}\mathrm {Na}{}^{}\mathrm {I}$
$<1.7 \times 10^{-10}$ 90 19
 2017 A
PNDX WIMPs on ${}^{}\mathrm {Xe}$
$<7.3 \times 10^{-7}$ 90
 2016
DS50 ${}^{}\mathrm {Ar}$
$<1 \times 10^{-5}$ 90 20
 2016
CDMS ${}^{}\mathrm {Ge}$
$<2 \times 10^{-4}$ 90 21
 2016
DMIC ${}^{}\mathrm {Si}$ CCDs
$<4.5 \times 10^{-5}$ 90 22
 2016
CRES ${}^{}\mathrm {CaWO}_{4}$
$<2 \times 10^{-6}$ 90 23
 2016
X100 ${}^{}\mathrm {Xe}$
$<9.4 \times 10^{-8}$ 90 24
 2016
EDE3 ${}^{}\mathrm {Ge}$
$<1.0 \times 10^{-7}$ 90 25
 2016
EDE3 ${}^{}\mathrm {Ge}$
$<5 \times 10^{-6}$ 90 26
 2016
CDEX ${}^{}\mathrm {Ge}$
$<1 \times 10^{-5}$ 90
 2015
DS50 ${}^{}\mathrm {Ar}$
$<1.5 \times 10^{-6}$ 90 27
 2015 A
CDM2 ${}^{}\mathrm {Ge}$
$<1.5 \times 10^{-7}$ 90 28
 2015 B
CDM2 ${}^{}\mathrm {Ge}$
$<2 \times 10^{-6}$ 90 29
 2015
PICO ${}^{}\mathrm {C}_{3}{}^{}\mathrm {F}_{8}$
$<1.2 \times 10^{-5}$ 90
 2015
SKAM ${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ ( ${{\mathit b}}{{\overline{\mathit b}}}$ )
$<1.19 \times 10^{-6}$ 90
 2015
SKAM ${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ ( ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ )
$<2 \times 10^{-8}$ 90 30
 2015
PNDX ${}^{}\mathrm {Xe}$
$<2.0 \times 10^{-7}$ 90 31
 2014
SCDM ${}^{}\mathrm {Ge}$
$<3.7 \times 10^{-5}$ 90 32
 2014 A
SCDM ${}^{}\mathrm {Ge}$
$<1 \times 10^{-9}$ 90 33
 2014
LUX ${}^{}\mathrm {Xe}$
$<2 \times 10^{-6}$ 90 34
 2014
CRES CaWO$_{4}$
$<5 \times 10^{-6}$ 90
 2014
SMPL C$_{2}$ClF$_{5}$
$<8 \times 10^{-6}$ 90 35
 2014 A
KIMS CsI
$<2 \times 10^{-4}$ 90 36
 2014 A
CDEX ${}^{}\mathrm {Ge}$
$<1 \times 10^{-5}$ 90 37
 2014
CDEX ${}^{}\mathrm {Ge}$
$<1.08 \times 10^{-4}$ 90 38
 2013
ICCB ${}^{}\mathrm {H}$, solar ${{\mathit \nu}}$ ( ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ )
$<1.5 \times 10^{-5}$ 90 39
 2013 B
XMAS ${}^{}\mathrm {Xe}$
$<3.1 \times 10^{-6}$ 90 40
 2013
CDM2 ${}^{}\mathrm {Si}$
$<3.4 \times 10^{-6}$ 90 41
 2013 A
CDM2 ${}^{}\mathrm {Si}$
$<2.2 \times 10^{-6}$ 90 42
 2013 A
CDM2 ${}^{}\mathrm {Si}$
43
 2013 A
DAMA ${}^{}\mathrm {Na}{}^{}\mathrm {I}$ modulation
$<1.2 \times 10^{-4}$ 90 44
 2013 B
TEXO ${}^{}\mathrm {Ge}$
45
 2013
CDEX ${}^{}\mathrm {Ge}$
$<1.2 \times 10^{-7}$ 90
 2012
ZEP3 ${}^{}\mathrm {Xe}$
46
 2012
CRES CaWO$_{4}$
$<8 \times 10^{-6}$ 90 47
 2012
CRES CaWO$_{4}$
$<7 \times 10^{-9}$ 90 48
 2012
X100 ${}^{}\mathrm {Xe}$
$<7 \times 10^{-7}$ 90 49
 2012
EDE2 ${}^{}\mathrm {Ge}$
50
 2012
DMIC CCD
$<2 \times 10^{-6}$ 90
 2012
COUP CF$_{3}$I
$<7 \times 10^{-6}$ 51
 2012
SMPL C$_{2}$ClF$_{5}$
$<1.5 \times 10^{-6}$ 90
 2012
KIMS CsI
$<5 \times 10^{-5}$ 90 52
 2011
CGNT ${}^{}\mathrm {Ge}$
53
 2011 A
CGNT ${}^{}\mathrm {Ge}$
$<5 \times 10^{-7}$ 90 54
 2011
CDM2 ${}^{}\mathrm {Ge}$, inelastic
$<2.7 \times 10^{-7}$ 90 55
 2011 A
RVUE ${}^{}\mathrm {Ge}$
$<3 \times 10^{-6}$ 90 56
 2011
XE10 ${}^{}\mathrm {Xe}$
$<7 \times 10^{-8}$ 90 57
 2011
X100 ${}^{}\mathrm {Xe}$
58
 2011 A
X100 ${}^{}\mathrm {Xe}$, inelastic
$<2 \times 10^{-8}$ 90 48
 2011 B
X100 ${}^{}\mathrm {Xe}$
59
 2011
ZEP3 ${}^{}\mathrm {Xe}$
$<2 \times 10^{-7}$ 90
 2010
CDM2 ${}^{}\mathrm {Ge}$
$<1 \times 10^{-5}$ 90 60
 2010
CDM2 ${}^{}\mathrm {Si}$, ${}^{}\mathrm {Ge}$, low threshold
$<1 \times 10^{-7}$ 90
 2010
X100 ${}^{}\mathrm {Xe}$
$<2 \times 10^{-6}$ 90
 2010
EDE2 ${}^{}\mathrm {Ge}$
$<4 \times 10^{-5}$ 90
 2010
SMPL C$_{2}$ClF$_{3}$
$<1.5 \times 10^{-7}$ 90 61
 2009
CDM2 ${}^{}\mathrm {Ge}$
$<2 \times 10^{-4}$ 90 62
 2009
TEXO ${}^{}\mathrm {Ge}$
63
 2008
CGNT ${}^{}\mathrm {Ge}$
 1 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.
 2 FELIZARDO 2020 presents 2014 SIMPLE bounds on WIMP DM using ${}^{}\mathrm {C}_{2}{}^{}\mathrm {Cl}{}^{}\mathrm {F}_{5}$ target .
 3 WANG 2020G search for SI WIMP scatter on ${}^{}\mathrm {Xe}$ with 132 t d exposure of PANDAX-II .
 4 ANGLOHER 2019 search for low mass WIMP scatter on ${}^{}\mathrm {Ca}{}^{}\mathrm {W}{}^{}\mathrm {O}_{4}$; no signal; limits placed on Wilson coefficients for m(${{\mathit \chi}}$ ) = $0.6 - 60$ GeV.
 5 KIM 2019A search for WIMP scatter in ${}^{}\mathrm {NaI}$ KIMS experiment; no signal: require ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit n}}$ ) $<$ $7 \times 10^{-5}$ pb for m(${{\mathit \chi}}$ ) = 20 GeV.
 6 KOBAYASHI 2019 search for WIMP scatter in XMASS single-phase liquid ${}^{}\mathrm {Xe}$ detector; no signal; require ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) $<$ $3 \times 10^{-7}$ pb for m(${{\mathit \chi}}$ ) = 20 GeV.
 7 SEONG 2019 search for ${{\mathit \Upsilon}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit A}}$ , ${{\mathit A}}$ $\rightarrow$ ${{\mathit \chi}}{{\mathit \chi}}$ via CP-odd Higgs; no signal; limits on BF set; model dependent conversion to WIMP-nucleon scattering cross section limits ${{\mathit \sigma}}{}^{SI}$ $<$ $10^{-36}$ cm${}^{2}$ for m(${{\mathit \chi}}$ ) = $0.01 - 1$ GeV.
 8 YANG 2019 search for low mass wimps via annual modulation in ${}^{}\mathrm {Ge}$; no signal; require ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) $<$ $3.5 \times 10^{-5}$ pb for m(${{\mathit \chi}}$ ) = 20 GeV.
 9 ABE 2018C search for WIMP annual modulation signal for m(WIMP): $6 - 20$ GeV; limits set on SI WIMP-nucleon cross section: see Fig. 6.
 10 ADHIKARI 2018 search for WIMP scatter on ${}^{}\mathrm {NaI}$; no signal; require ${{\mathit \sigma}}{}^{SI}$ $<$ $1.44 \times 10^{-5}$ pb for m(WIMP) = 20 GeV; inconsistent with DAMA/LIBRA result.
 11 AGNES 2018 search low mass m(WIMP): $1.8 - 20$ GeV scatter on ${}^{}\mathrm {Ar}$; limits on SI WIMP-nucleon cross section set in Fig. 8.
 12 AGNESE 2018 give limits for ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) for m(WIMP) between 1.5 and 20 GeV using CDMSlite mode data.
 13 AGNESE 2018A search for WIMP scatter on Ge at SuperCDMS; 1 event, consistent with expected background; set limit in ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) vs. m(${{\mathit \chi}}$ ) plane for m $\sim{}$ $10 - 250$ GeV.
 14 APRILE 2018 search for WIMP scatter on 1 t yr ${}^{}\mathrm {Xe}$; no signal, limits placed in ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) vs. m(${{\mathit \chi}}$ ) plane for m(${{\mathit \chi}}$ ) $\sim{}$ $6 - 1000$ GeV.
 15 ARNAUD 2018 search for low mass WIMP scatter on ${}^{}\mathrm {Ne}$ via SPC at NEWS-G; limits set in ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) vs. m(${{\mathit \chi}}$ ) plane for m $\sim{}$ $0.5 - 20$ GeV.
 16 AARTSEN 2017 obtain ${\mathit \sigma (}SI{)}$ $<$ $6 \times 10^{-6}$ pb for m(wimp) = 20 GeV from ${{\mathit \nu}}$ from earth.
 17 AKERIB 2017 search for WIMP scatter on ${}^{}\mathrm {Xe}$; 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.
 18 BARBOSA-DE-SOUZA 2017 search for annual modulation of WIMP scatter on ${}^{}\mathrm {Na}{}^{}\mathrm {I}$ using an exposure of 61 kg yr of DM-Ice17 for recoil energy in the $4 - 20$ keV range (DAMA found modulation for recoil energy $<$ 5 keV). No modulation seen. Sensitivity insufficient to distinguish DAMA signal from null.
 19 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 ${}^{}\mathrm {Xe}$.
 20 AGNESE 2016 CDMSlite excludes low mass WIMPs $1.6 - 5.5$ GeV and SI scattering cross section depending on $\mathit m$(WIMP); see Fig. 4.
 21 AGUILAR-AREVALO 2016 search low mass $1 - 10$ GeV WIMP scatter on ${}^{}\mathrm {Si}$ CCDs; set limits Fig. 11.
 22 ANGLOHER 2016 search for GeV scale WIMP scatter on ${}^{}\mathrm {CaWO}_{4}$; limits placed in ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) vs. m(${{\mathit \chi}}$ ) plane for m(${{\mathit \chi}}$ ) $\sim{}$ $0.5 - 30$ GeV.
 23 APRILE 2016 search for low mass WIMPs via ionization at XENON100; limits placed in ${{\mathit \sigma}}{}^{SI}$( ${{\mathit \chi}}{{\mathit N}}$ ) vs m(${{\mathit \chi}}$ ) plane for m $\sim{}$ $3.5 - 20$ GeV.
 24 ARMENGAUD 2016 search for GeV scale WIMP scatter on ${}^{}\mathrm {Ge}$; limits placed in ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) vs. m(${{\mathit \chi}}$ ) plane for m(${{\mathit \chi}}$ ) $\sim{}$ $4 - 30$ GeV.
 25 HEHN 2016 search for low mass WIMPs via SI scatter on ${}^{}\mathrm {Ge}$ target using profile likelihood analysis; limits placed in ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) vs. m(${{\mathit \chi}}$ ) plane for m(${{\mathit \chi}}$ ) $\sim{}$ $4 - 30$ GeV.
 26 ZHAO 2016 search for GeV-scale WIMP scatter on ${}^{}\mathrm {Ge}$; limits placed in ${{\mathit \sigma}^{SI}}$ ( ${{\mathit \chi}}{{\mathit N}}$ ) vs. m(${{\mathit \chi}}$ ) plane for m(${{\mathit \chi}}$ ) $\sim{}$ $4 - 30$ GeV.
 27 AGNESE 2015A reanalyse AHMED 2011B low threshold data. See their Fig. 12 (left) for improved limits extending down to 5 GeV.
 28 AGNESE 2015B reanalyse AHMED 2010 data.
 29 See their Fig. 7 for limits extending down to 4 GeV.
 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 This limit value is provided by the authors. See their Fig. 4 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 3.5 GeV.
 32 This limit value is provided by the authors. AGNESE 2014A result is from CDMSlite mode operation with enhanced sensitivity to low mass ${\mathit m}_{{{\mathit X}^{0}}}$. See their Fig. 3 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 3.5 GeV (see also Fig. 4 in AGNESE 2014 ).
 33 See their Fig. 5 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 5.5 GeV.
 34 See their Fig. 5 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 1 GeV.
 35 See their Fig. 5 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 5 GeV.
 36 LIU 2014A result is based on prototype CDEX-0 detector. See their Fig. 13 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 2 GeV.
 37 See their Fig. 4 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 4.5 GeV.
 38 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.
 39 See their Fig. 8 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 7 GeV.
 40 This limit value is provided by the authors. AGNESE 2013 use data taken between Oct. 2006 and July 2007. See their Fig. 4 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 7 GeV.
 41 This limit value is provided by the authors. AGNESE 2013A use data taken between July 2007 and Sep. 2008. Three candidate events are seen. Assuming these events are real, the best fit parameters are ${\mathit m}_{{{\mathit X}^{0}}}$ = 8.6 GeV and $\sigma$ = $1.9 \times 10^{-5}$ pb.
 42 This limit value is provided by the authors. Limit from combined data of AGNESE 2013 and AGNESE 2013A. See their Fig. 4 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 5.5 GeV.
 43 BERNABEI 2013A search for annual modulation of counting rate in the $2 - 6$ keV recoil energy interval, in a 14 yr live time exposure of 1.33 t yr. Find a modulation of $0.0112$ $\pm0.0012$ counts/(day kg keV) with 9.3 sigma C.L. Find period and phase in agreement with expectations from DM particles.
 44 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.
 45 See their Fig. 5 for limits for ${\mathit m}_{{{\mathit X}^{0}}}$ = $4 - 12$ GeV.
 46 ANGLOHER 2012 observe excess events above the expected background which are consistent with ${{\mathit X}^{0}}$ with mass $\sim{}$ 25 GeV (or 12 GeV) and spin-independent ${{\mathit X}^{0}}$ -nucleon cross section of $2 \times 10^{-6}$ pb (or $4 \times 10^{-5}$ pb).
 47 Reanalysis of ANGLOHER 2009 data with all three nuclides. See also BROWN 2012 .
 49 See their Fig. 4 for limits extending down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 7 GeV.
 50 See their Fig. 13 for cross section limits for ${\mathit m}_{{{\mathit X}^{0}}}$ between 1.2 and 10 GeV.
 52 See their Fig. 4 for limits extending to ${\mathit m}_{{{\mathit X}^{0}}}$ = 3.5 GeV.
 53 AALSETH 2011A find indications of annual modulation of the data, the energy spectrum being compatible with ${{\mathit X}^{0}}$ mass around 8 GeV. See also AALSETH 2013 .
 54 AHMED 2011 search for ${{\mathit X}^{0}}$ inelastic scattering. See their Fig. $8 - 10$ for limits. The inelastic cross section reduces to the elastic cross section at the limit of zero mass splitting (Fig. 8, left).
 55 AHMED 2011A combine CDMS II and EDELWEISS data.
 56 ANGLE 2011 show limits down to ${\mathit m}_{{{\mathit X}^{0}}}$ = 4 GeV on Fig. 3.
 57 APRILE 2011 reanalyze APRILE 2010 data.
 58 APRILE 2011A search for ${{\mathit X}^{0}}$ inelastic scattering. See their Fig. 2 and 3 for limits. See also APRILE 2014A.
 59 HORN 2011 perform detector calibration by neutrons. Earlier results are only marginally affected.
 60 See their Fig. 10 and 12 for limits extending to ${{\mathit X}^{0}}$ mass of 1 GeV.
 61 Superseded by AHMED 2010 .
 62 See their Fig. 6(a) for cross section limits for ${\mathit m}_{{{\mathit X}^{0}}}$ extending down to 2 GeV.
 63 See their Fig. 2 for cross section limits for ${\mathit m}_{{{\mathit X}^{0}}}$ between 4 and 10 GeV.
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