³⁴ **ABBEDIENDI** 99P search for s-channel graviton exchange effects in $e^+e^- \to \gamma\gamma$ at $E_{cm}=189$ GeV. The limits $G_+ > 660$ GeV and $G_- > 634$ GeV are obtained from combined $E_{cm}=183$ and 189 GeV data, where $G_\pm$ is a scale related to the fundamental gravity scale.

³⁵ **ACCIARRI** 99M search for the reaction $e^+e^- \to \gamma G$ and s-channel graviton exchange effects in $e^+e^- \to \gamma\gamma$, $W^+W^-$, $ZZ$, $e^+e^-$, $\mu^+\mu^-$, $\tau^+\tau^-$, $q\bar{q}$ at $E_{cm}=183$ GeV. Limits on the gravity scale are listed in their Tables 1 and 2.

³⁶ **ACCIARRI** 99S search for the reaction $e^+e^- \to ZG$ and s-channel graviton exchange effects in $e^+e^- \to \gamma\gamma$, $W^+W^-$, $ZZ$, $e^+e^-$, $\mu^+\mu^-$, $\tau^+\tau^-$, $q\bar{q}$ at $E_{cm}=189$ GeV. Limits on the gravity scale are listed in their Tables 1 and 2.

³⁷ **BOURILKOV** 99 performs global analysis of LEP data on $e^+e^-$ collisions at $\sqrt{s}=183$ and 189 GeV. Bound is on $\Lambda_T$.

## Limits on $1/R = M_c$

This section includes limits on $1/R = M_c$, the compactification scale in models with one TeV-sized extra dimension, due to exchange of Standard Model KK excitations. Bounds assume fermions are not in the bulk, unless stated otherwise. See the "Extra Dimensions" review for discussion of model dependence.

<table><thead><tr><th>VALUE (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td rowspan="2">&gt;4.16</td><td rowspan="2">95</td><td>1 AAD</td><td>12CC ATLS</td><td>pp → ℓℓ</td></tr><tr><td>2 BARBIERI</td><td>04 RVUE</td><td>Electroweak</td></tr><tr><td>&gt;6.1</td><td></td><td></td><td></td><td></td></tr><tr><td colspan="5">● ● ● We do not use the following data for averages, fits, limits, etc. ● ● ●</td></tr><tr><td></td><td></td><td>3 FLORES</td><td>23 RVUE</td><td>minimal universal extra dims</td></tr><tr><td></td><td></td><td>4 AVNISH</td><td>21 RVUE</td><td>pp → multijet</td></tr><tr><td></td><td></td><td>5 AABOUD</td><td>18AV ATLS</td><td>pp → t<span style="text-decoration: overline">t</span>t<span style="text-decoration: overline">t</span></td></tr><tr><td></td><td></td><td>6 AABOUD</td><td>18CE ATLS</td><td>pp → t<span style="text-decoration: overline">t</span>t<span style="text-decoration: overline">t</span></td></tr><tr><td>&gt;3.8</td><td>95</td><td>7 ACCOMANDO 15</td><td>RVUE</td><td>Electroweak</td></tr><tr><td>&gt;3.40</td><td>95</td><td>8 KHACHATRY..15T</td><td>CMS</td><td>pp → ℓX</td></tr><tr><td></td><td></td><td>9 CHATRCHYAN 13AQ</td><td>CMS</td><td>pp → ℓX</td></tr><tr><td>&gt;1.38</td><td>95</td><td>10 CHATRCHYAN 13W</td><td>CMS</td><td>pp → γγ, δ=6, M<sub>D</sub>=5 TeV</td></tr><tr><td>&gt;0.715</td><td>95</td><td>11 EDELHAUSER 13</td><td>RVUE</td><td>pp → ℓ<span style="text-decoration: overline">t</span> + X</td></tr><tr><td>&gt;1.40</td><td>95</td><td>12 AAD</td><td>12CP ATLS</td><td>pp → γγ, δ=6, M<sub>D</sub>=5 TeV</td></tr><tr><td>&gt;1.23</td><td>95</td><td>13 AAD</td><td>12X ATLS</td><td>pp → γγ, δ=6, M<sub>D</sub>=5 TeV</td></tr><tr><td>&gt;0.26</td><td>95</td><td>14 ABAZOV</td><td>12M D0</td><td>p<span style="text-decoration: overline">p</span> → µµ</td></tr><tr><td>&gt;0.75</td><td>95</td><td>15 BAAK</td><td>12 RVUE</td><td>Electroweak</td></tr><tr><td></td><td></td><td>16 FLACKE</td><td>12 RVUE</td><td>Electroweak</td></tr><tr><td>&gt;0.43</td><td>95</td><td>17 NISHIWAKI</td><td>12 RVUE</td><td>H → WW, γγ</td></tr><tr><td>&gt;0.729</td><td>95</td><td>18 AAD</td><td>11F ATLS</td><td>pp → γγ, δ=6, M<sub>D</sub>=5 TeV</td></tr><tr><td>&gt;0.961</td><td>95</td><td>19 AAD</td><td>11X ATLS</td><td>pp → γγ, δ=6, M<sub>D</sub>=5 TeV</td></tr><tr><td>&gt;0.477</td><td>95</td><td>20 ABAZOV</td><td>10P D0</td><td>p<span style="text-decoration: overline">p</span> → γγ, δ=6, M<sub>D</sub>=5 TeV</td></tr><tr><td>&gt;1.59</td><td>95</td><td>21 ABAZOV</td><td>09AE D0</td><td>p<span style="text-decoration: overline">p</span> → dijet, angular dist.</td></tr><tr><td>&gt;0.6</td><td>95</td><td>22 HAISCH</td><td>07 RVUE</td><td>B → X<sub>S</sub>γ</td></tr><tr><td>&gt;0.6</td><td>90</td><td>23 GOGOLADZE</td><td>06 RVUE</td><td>Electroweak</td></tr><tr><td>&gt;3.3</td><td>95</td><td>24 CORNET</td><td>00 RVUE</td><td>Electroweak</td></tr><tr><td>&gt;3.3-3.8</td><td>95</td><td>25 RIZZO</td><td>00 RVUE</td><td>Electroweak</td></tr></tbody></table>

¹ AAD 12CC use 4.9 and 5.0 fb⁻¹ of data from pp collisions at $\sqrt{s} = 7$ TeV in the dielectron and dimuon channels, respectively, to place a lower bound on the mass of the lightest KK $Z/\gamma$ boson (equivalent to $1/R = M_c$). The limit quoted here assumes a flat prior corresponding to when the pure $Z/\gamma$ KK cross section term dominates. See their Section 15 for more details.

² **BARBIERI** 04 use electroweak precision observables to place a lower bound on the compactification scale $1/R$. Both the gauge bosons and the Higgs boson are assumed to propagate in the bulk.

³ **FLORES** 23 use a number of 13 TeV Run 2 searches at the LHC to place constraints on the compactification scale $1/R$ and cutoff scale $\Lambda$ in the minimal universal extra dimension model with Standard Model fields propagating in the bulk (see their Fig. 6).

⁴ **AVNISH** 21 perform a study on the ATLAS collaboration search for multiple jets plus missing transverse energy from pp collisions at $\sqrt{s} = 13$ TeV and integrated luminosity of 139 fb⁻¹, to place constraints on the compactification scale and cutoff scale $\Lambda$ in universal extra dimension models with Standard Model fields propagating in the bulk.

⁵ **AABOUD** 18AV use 36.1 fb⁻¹ of data from pp collisions at $\sqrt{s} = 13$ TeV in final states with multiple b-jets, to place a lower bound on the compactification scale in a model with two universal extra dimensions. Assuming the radii of the two extra dimensions are equal, a lower limit of 1.8 TeV for the Kaluza-Klein mass is obtained.

⁶ **AABOUD** 18CE use 36.1 fb⁻¹ of data from pp collisions at $\sqrt{s} = 13$ TeV in final states with same-charge leptons and b-jets, to place a lower bound on the compactification scale in a model with two universal extra dimensions. Assuming the radii of the two extra dimensions are equal, a lower limit of 1.45 TeV for the Kaluza-Klein mass is obtained.

⁷ **ACCOMANDO** 15 use electroweak precision observables to place a lower bound on the compactification scale $1/R$. See their Fig. 2. For the bound as a function of $\sin\beta$, which parametrizes the VEV contribution from brane and bulk Higgs fields. The quoted value is for the minimum bound which occurs at $\sin\beta = 0.45$.

⁸ **KHACHATRYAN** 15T use 19.7 fb⁻¹ of data from pp collisions at $\sqrt{s} = 8$ TeV to place a lower bound on the compactification scale $1/R$.

⁹ **CHATRCHYAN** 13AQ use 5.0 fb⁻¹ of data from pp collisions at $\sqrt{s} = 7$ TeV and a further 3.7 fb⁻¹ of data at $\sqrt{s} = 8$ TeV to place a lower bound on the compactification scale $1/R$, in models with universal extra dimensions and Standard Model fields propagating in the bulk. See their Fig. 5 for the bound as a function of the universal bulk fermion mass parameter $\mu$.

¹⁰ **CHATRCHYAN** 13W use diphoton events with large missing transverse momentum in 4.93 fb⁻¹ of data produced from pp collisions at $\sqrt{s} = 7$ TeV to place a lower bound on the compactification scale in a universal extra dimension model with gravitational decays. The bound assumes that the cutoff scale $\Lambda$, for the radiative corrections to the Kaluza-Klein masses, satisfies $\Lambda/M_c = 20$. The model parameters are chosen such that the decay $\gamma^* \to G\gamma$ occurs with an appreciable branching fraction.

¹¹ **EDELHAUSER** 13 use 19.6 and 20.6 fb⁻¹ of data from pp collisions at $\sqrt{s} = 8$ TeV analyzed by the CMS Collaboration in the dielectron and dimuon channels, respectively, to place a lower bound on the mass of the second lightest Kaluza-Klein $Z/\gamma$ boson (converted to a limit on $1/R = M_c$). The bound assumes Standard Model fields propagating

in the bulk and that the cutoff scale $\Lambda$, for the radiative corrections to the Kaluza-Klein masses, satisfies $\Lambda/M_c = 20$.

¹² **AAD** 12CP use diphoton events with large missing transverse momentum in 4.8 fb⁻¹ of data produced from pp collisions at $\sqrt{s} = 7$ TeV to place a lower bound on the compactification scale in a universal extra dimension model with gravitational decays. The bound assumes that the cutoff scale $\Lambda$, for the radiative corrections to the Kaluza-Klein masses, satisfies $\Lambda/M_c = 20$. The model parameters are chosen such that the decay $\gamma^* \to G\gamma$ occurs with an appreciable branching fraction.

¹³ **AAD** 12X use diphoton events with large missing transverse momentum in 1.07 fb⁻¹ of data produced from pp collisions at $\sqrt{s} = 7$ TeV to place a lower bound on the compactification scale in a universal extra dimension model with gravitational decays. The bound assumes that the cutoff scale $\Lambda$, for the radiative corrections to the Kaluza-Klein masses, satisfies $\Lambda/M_c = 20$. The model parameters are chosen such that the decay $\gamma^* \to G\gamma$ occurs with an appreciable branching fraction.

¹⁴ **ABAZOV** 12M use same-sign dimuon events in 7.3 fb⁻¹ of data from p<span style="text-decoration: overline">p</span> collisions at $\sqrt{s} = 1.96$ TeV to place a lower bound on the compactification scale $1/R$, in models with universal extra dimensions where all Standard Model fields propagate in the bulk.

¹⁵ **BAAK** 12 use electroweak precision observables to place a lower bound on the compactification scale $1/R$, in models with universal extra dimensions and Standard Model fields propagating in the bulk. Bound assumes a 125 GeV Higgs mass. See their Fig. 25 for the bound as a function of the Higgs mass.

¹⁶ **FLACKE** 12 use electroweak precision observables to place a lower bound on the compactification scale $1/R$, in models with universal extra dimensions and Standard Model fields propagating in the bulk. See their Fig. 1 for the bound as a function of the universal bulk fermion mass parameter $\mu$.

¹⁷ **NISHIWAKI** 12 use up to 2 fb⁻¹ of data from the ATLAS and CMS experiments that constrains the production cross section of a Higgs-like particle to place a lower bound on the compactification scale $1/R$ in universal extra dimension models. The quoted bound assumes Standard Model fields propagating in the bulk and a 125 GeV Higgs mass. See their Fig. 1 for the bound as a function of the Higgs mass.

¹⁸ **AAD** 11F use diphoton events with large missing transverse energy in 3.1 pb⁻¹ of data produced from pp collisions at $\sqrt{s} = 7$ TeV to place a lower bound on the compactification scale in a universal extra dimension model with gravitational decays. The bound assumes that the cutoff scale $\Lambda$, for the radiative corrections to the Kaluza-Klein masses, satisfies $\Lambda/M_c = 20$. The model parameters are chosen such that the decay $\gamma^* \to G\gamma$ occurs with an appreciable branching fraction.

¹⁹ **AAD** 11X use diphoton events with large missing transverse energy in 36 fb⁻¹ of data produced from pp collisions at $\sqrt{s} = 7$ TeV to place a lower bound on the compactification scale in a universal extra dimension model with gravitational decays. The bound assumes that the cutoff scale $\Lambda$, for the radiative corrections to the Kaluza-Klein masses, satisfies $\Lambda/M_c = 20$. The model parameters are chosen such that the decay $\gamma^* \to G\gamma$ occurs with an appreciable branching fraction.

²⁰ **ABAZOV** 10P use diphoton events with large missing transverse energy in 6.3 fb⁻¹ of data produced from p<span style="text-decoration: overline">p</span> collisions at $\sqrt{s} = 1.96$ TeV to place a lower bound on the compactification scale in a universal extra dimension model with gravitational decays. The bound assumes that the cutoff scale $\Lambda$, for the radiative corrections to the Kaluza-Klein masses, satisfies $\Lambda/M_c = 20$. The model parameters are chosen such that the decay $\gamma^* \to G\gamma$ occurs with an appreciable branching fraction.

²¹ **ABAZOV** 09AE use dijet angular distributions in 0.7 fb⁻¹ of data from p<span style="text-decoration: overline">p</span> collisions at $\sqrt{s} = 1.96$ TeV to place a lower bound on the compactification scale.

²² **HAISCH** 07 use inclusive B-meson decays to place a Higgs mass independent bound on the compactification scale $1/R$ in the minimal universal extra dimension model.

²³ **GOGOLADZE** 06 use electroweak precision observables to place a lower bound on the compactification scale in models with universal extra dimensions. Bound assumes a 115 GeV Higgs mass. See their Fig. 3 for the bound as a function of the Higgs mass.

²⁴ **CORNET** 00 translates a bound on the coefficient of the 4-fermion operator $(\bar{t}\gamma^\mu\tau^A\ell)(\bar{t}\gamma^\mu\tau^A\ell)$ derived by Hagiwara and Matsumoto into a limit on the mass scale of KK W bosons.

²⁵ **RIZZO** 00 obtains limits from global electroweak fits in models with a Higgs in the bulk (3.8 TeV) or on the standard brane (3.3 TeV).

## Limits on Kaluza-Klein Gravitons in Warped Extra Dimensions

This section places limits on the mass of the first Kaluza-Klein (KK) excitation of the graviton in the warped extra dimension model of Randall and Sundrum. Bounds in parenthesis assume Standard Model fields propagate in the bulk. Experimental bounds depend strongly on the warp parameter, $k$. See the "Extra Dimensions" review for a full discussion.

Here we list limits for the value of the warp parameter $k/M_P = 0.1$.

<table><thead><tr><th>VALUE (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td rowspan="2">&gt;4.78</td><td rowspan="2">95</td><td>1 SIRUNYAN</td><td>21N CMS</td><td>pp → G → e<sup>+</sup>e<sup>-</sup>, µ<sup>+</sup>µ<sup>-</sup></td></tr><tr><td>2 TUMASYAN</td><td>23AP CMS</td><td>pp → G → WW, ZZ</td></tr><tr><td rowspan="10">&gt;2.6</td><td rowspan="10">95</td><td>3 AAD</td><td>22F ATLS</td><td>pp → G → HH</td></tr><tr><td>4 TUMASYAN</td><td>22D CMS</td><td>pp → G → WW</td></tr><tr><td>5 TUMASYAN</td><td>22J CMS</td><td>pp → G → ZZ</td></tr><tr><td>6 TUMASYAN</td><td>22R CMS</td><td>pp → G → ZZ</td></tr><tr><td>7 TUMASYAN</td><td>22U CMS</td><td>pp → G → HH</td></tr><tr><td>8 AAD</td><td>21AF ATLS</td><td>pp → G → ZZ</td></tr><tr><td>9 AAD</td><td>21AY ATLS</td><td>pp → G → γγ</td></tr><tr><td>10 AAD</td><td>20AT ATLS</td><td>pp → G → WW, ZZ</td></tr><tr><td>11 AAD</td><td>20C ATLS</td><td>pp → G → HH</td></tr><tr><td>12 AAD</td><td>20T ATLS</td><td>pp → G → b<span style="text-decoration: overline">b</span></td></tr><tr><td>13 SIRUNYAN</td><td>20AI CMS</td><td>pp → G → j<span style="text-decoration: overline">j</span></td></tr><tr><td>14 SIRUNYAN</td><td>20F CMS</td><td>pp → G → HH</td></tr><tr><td>15 AABOUD</td><td>19O ATLS</td><td>pp → G → HH</td></tr><tr><td>16 AAD</td><td>19D ATLS</td><td>pp → G → WW, ZZ</td></tr><tr><td>17 SIRUNYAN</td><td>19C CMS</td><td>pp → G → HH</td></tr><tr><td>18 SIRUNYAN</td><td>19BE CMS</td><td>pp → G → HH</td></tr><tr><td>19 AABOUD</td><td>18BI ATLS</td><td>pp → G → t<span style="text-decoration: overline">t</span></td></tr><tr><td>20 AABOUD</td><td>18CJ ATLS</td><td>pp → G → V<span style="text-decoration: overline">V</span>,V<span style="text-decoration: overline">H</span>,t<span style="text-decoration: overline">t</span></td></tr></tbody></table>
# Searches Particle Listings

## Extra Dimensions

<table><tbody><tr><td rowspan="15">&gt;4.1</td><td rowspan="15">95</td><td>21 AABOUD</td><td>18CQ ATLS</td><td>pp → G → HH</td></tr><tr><td>22 AABOUD</td><td>18CW ATLS</td><td>pp → G → HH</td></tr><tr><td>23 SIRUNYAN</td><td>18AF CMS</td><td>pp → G → HH</td></tr><tr><td>24 SIRUNYAN</td><td>18AS CMS</td><td>pp → G → ZZ</td></tr><tr><td>25 SIRUNYAN</td><td>18CW CMS</td><td>pp → G → HH</td></tr><tr><td>26 SIRUNYAN</td><td>18DU CMS</td><td>pp → G → γγ</td></tr><tr><td>27 SIRUNYAN</td><td>18I CMS</td><td>pp → G → b<span style="text-decoration: overline">b</span></td></tr><tr><td>28 AAD</td><td>16R ATLS</td><td>pp → G → WW, ZZ</td></tr><tr><td>29 AAD</td><td>15AZ ATLS</td><td>pp → G → WW</td></tr><tr><td>30 AAD</td><td>15CP ATLS</td><td>pp → G → WW, ZZ</td></tr><tr><td>31 AAD</td><td>14V ATLS</td><td>pp → G → e<sup>+</sup>e<sup>−</sup>, μ<sup>+</sup>μ<sup>−</sup></td></tr><tr><td>32 AAD</td><td>13A ATLS</td><td>pp → G → WW</td></tr><tr><td>33 AAD</td><td>13AO ATLS</td><td>pp → G → WW</td></tr><tr><td>34 AAD</td><td>13AS ATLS</td><td>pp → γγ, e<sup>+</sup>e<sup>−</sup>, μ<sup>+</sup>μ<sup>−</sup></td></tr><tr><td>35 AAD</td><td>12AD ATLS</td><td>pp → G → ZZ</td></tr><tr><td>36 AALTONEN</td><td>12V CDF</td><td>p<span style="text-decoration: overline">p</span> → G → ZZ</td></tr><tr><td>37 BAAK</td><td>12 RVUE</td><td>Electroweak</td></tr><tr><td>38 AALTONEN</td><td>116 CDF</td><td>p<span style="text-decoration: overline">p</span> → G → ZZ</td></tr><tr><td>39 AALTONEN</td><td>11R CDF</td><td>p<span style="text-decoration: overline">p</span> → G → e<sup>+</sup>e<sup>−</sup>, γγ</td></tr><tr><td>40 ABAZOV</td><td>11H D0</td><td>p<span style="text-decoration: overline">p</span> → G → WW</td></tr><tr><td>41 AALTONEN</td><td>10N CDF</td><td>p<span style="text-decoration: overline">p</span> → G → WW</td></tr><tr><td>42 ABAZOV</td><td>10F D0</td><td>p<span style="text-decoration: overline">p</span> → G → e<sup>+</sup>e<sup>−</sup>, γγ</td></tr><tr><td>43 AALTONEN</td><td>08S CDF</td><td>p<span style="text-decoration: overline">p</span> → G → ZZ</td></tr><tr><td>44 ABAZOV</td><td>08J D0</td><td>p<span style="text-decoration: overline">p</span> → G → e<sup>+</sup>e<sup>−</sup>, γγ</td></tr><tr><td>45 AALTONEN</td><td>07G CDF</td><td>p<span style="text-decoration: overline">p</span> → G → γγ</td></tr><tr><td>46 AALTONEN</td><td>07H CDF</td><td>p<span style="text-decoration: overline">p</span> → G → e<span style="text-decoration: overline">e</span></td></tr><tr><td>47 ABAZOV</td><td>05N D0</td><td>p<span style="text-decoration: overline">p</span> → G → ℓℓ, γγ</td></tr><tr><td>48 ABULENCIA</td><td>05A CDF</td><td>p<span style="text-decoration: overline">p</span> → G → ℓℓ</td></tr></tbody></table>

1 SIRUNYAN 21N use 137 (140) fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for dilepton resonances in the dielectron (dimonium) channel. See Table 6 for other limits with warp parameter values $k/M_P$ = 0.01 and 0.05. This updates the results of SIRUNYAN 18Bb.

2 TUMASYAN 23AP use 138 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for $WW, ZZ$ diboson resonances in $q\bar{q}q\bar{q}$ final states. See their Figure 7 for the limit on the cross section times branching fraction as a function of the KK graviton mass. Assuming $k/M_P$ = 0.5, a graviton mass is excluded below 1400 GeV. This updates the result of SIRUNYAN 20q.

3 AAD 22r use 126-139 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}b\bar{b}$ final state. See their Figure 14 for limits on the cross section times branching fraction as a function of the KK graviton mass. Assuming $k/M_P$ = 1, gravitons in the mass range 298-1460 GeV are excluded. This updates the results of AABOUD 19a.

4 TUMASYAN 22d use 137 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for $WW$ resonances in $t\bar{t}q\bar{q}$ final states ($\ell = e, \mu$). See their Figure 6 for the limit on the KK graviton mass as a function of the cross section times branching fraction, including theoretical values for $k/M_P$ = 0.5. This updates the results of SIRUNYAN 18AX.

5 TUMASYAN 22j use 137 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for $ZZ$ resonances in $\nu\bar{\nu}q\bar{q}$ final state. See their Figure 10 for the limit on the KK graviton mass as a function of the cross section times branching fraction, assuming $k/M_P$ = 0.5. This updates the result of SIRUNYAN 18Bk.

6 TUMASYAN 22R use 138 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for $ZZ$ resonances in $\ell'\ell'q$ final states ($\ell = e, \mu$). See their Figure 8 for the limit on the KK graviton mass as a function of the cross section times branching fraction. Assuming $k/M_P$ = 0.5, a graviton mass is excluded below 1200 GeV. This updates the result of SIRUNYAN 18D.

7 TUMASYAN 22U use 138 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}q\bar{q}$, $b\bar{b}\ell\ell\nu$ and $b\bar{b}\nu\ell\nu\ell\nu$ final states ($\ell = e, \mu$). See their Figure 7 for limits on the cross section times branching fraction as a function of the KK graviton mass, including theoretical values for $k/M_P$ = 0.3 and 0.5. This updates the results of SIRUNYAN 19CF and SIRUNYAN 18F.

8 AAD 21AF use 139 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for $ZZ$ resonances in the $\ell'\ell'\ell$ and $\ell'\ell\nu\nu$ final states ($\ell = e, \mu$). See their Figure 8 for the limit on the cross section times branching fraction as a function of the KK graviton mass, including theoretical values for $k/M_P$ = 1. This updates the results of AAD 15AU and AABOUD 18Bb.

9 AAD 21AY use 139 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV in the diphoton channel to place a lower limit on the mass of the lightest KK graviton. This updates the results of AABOUD 17Aa.

10 AAD 20AT use 139 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for diboson resonances in semileptonic final states ($\ell\nu q\bar{q}, \ell\nu\nu q\bar{q}$). See their Figure 15 for the limit on the cross section times branching fraction as a function of the KK graviton mass. Lower limits on the graviton mass are also given for $k/M_P$ = 1. This updates the results of AABOUD 18AK and AABOUD 18AL.

11 AAD 20c use 139 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}b\bar{b}$, $b\bar{b}W^+W^-$, and $b\bar{b}\tau^+\tau^-$ final states. See their Figure 5(b)(c) for limits on the cross section as a function of the KK graviton mass. In the case of $k/M_P$ = 1 and 2, gravitons are excluded in the mass range 260-3000 GeV and 260-1760 GeV, respectively.

12 SIRUNYAN 20AI use 137 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for dijet resonances. See their Figure 6 for the limit on the product of the cross section, branching fraction, acceptance and b-tagging efficiency as a function of the KK graviton mass. In the case of $k/M_P$ = 0.2, KK gravitons in the mass range 1.25-2.8 TeV are excluded.

13 SIRUNYAN 20F use 35.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}ZZ$ final state. See their Figure 4 for limits on the cross section times branching fraction as a function of the KK graviton mass, and Figure 5 for limits as a function of $k/M_P$.

14 AABOUD 19O use 36.1 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}WW$ final state. See their Figure 12 for limits

on the cross section times branching fraction as a function of the KK graviton mass for $k/M_P$ = 1 and $k/M_P$ = 2.

16 AAD 19D use 139 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for diboson resonances in the all-hadronic final state. See their Figure 9(b) for the limit on the cross section times branching fraction as a function of the KK graviton mass, including theoretical values for $k/M_P$ = 1. This updates the results of AABOUD 18F.

17 SIRUNYAN 19 use 35.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $\gamma\gamma b\bar{b}$ final state. See their Figure 9 for limits on the cross section times branching fraction as a function of the KK graviton mass. Assuming $k/M_P$ = 1, gravitons in the mass range 290-810 GeV are excluded. This updates the result of KHACHATRYAN 16Bq.

18 SIRUNYAN 19B use 35.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production by combining the results from four final states: $b\bar{b}\gamma\gamma, b\bar{b}\tau^+\tau^-$, $b\bar{b}b\bar{b}$, and $b\bar{D}V\nu$. See their Figure 7 for limits on the cross section times branching fraction as a function of the KK graviton mass.

19 AABOUD 18BI use 36.1 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for top-quark pairs decaying into the lepton-plus jets topology. See their Figure 16 for the limit on the KK graviton mass as a function of the cross section times branching fraction, including theoretical values for $k/M_P$ = 1.

20 AABOUD 18CJ combine the searches for heavy resonances decaying into bosonic and leptonic final states from 36.1 fb⁻¹ of pp collision data at $\sqrt{s}$ = 13 TeV. The lower limit on the KK graviton mass, with $k/M_P$ = 1, is 2.3 TeV.

21 AABOUD 18CQ use 36.1 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}\tau^+\tau^-$ final state. See their Figure 2 for limits on the cross section times branching fraction as a function of the KK graviton mass. Assuming $k/M_P$ = 1, gravitons in the mass range 325-885 GeV are excluded.

22 AABOUD 18CW use 36.1 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $\gamma\gamma b\bar{b}$ final state. See their Figure 7 for limits on the cross section times branching fraction as a function of the KK graviton mass.

23 SIRUNYAN 18AF use 35.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}b\bar{b}$ final state. See their Figure 9 for limits on the cross section times branching fraction as a function of the KK graviton mass, including theoretical values for $k/M_P$ = 0.5. This updates the results of KHACHATRYAN 15R.

24 SIRUNYAN 18AS use 35.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for $ZZ$ resonances in the $\ell'\ell\nu\nu$ final state ($\ell = e, \mu$). See their Figure 5 for the limit on the KK graviton mass as a function of the cross section times branching fraction, including theoretical values for $k/M_P$ = 0.1, 0.5, and 1.0.

25 SIRUNYAN 18CW use 35.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV to search for Higgs boson pair production in the $b\bar{b}b\bar{b}$ final state. See their Figure 8 for limits on the cross section times branching fraction as a function of the KK graviton mass, including theoretical values for $k/M_P$ = 0.5.

26 SIRUNYAN 18DU use 35.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 13 TeV, in the diphoton channel to place a lower limit on the mass of the lightest KK graviton. See their paper for limits with other warp parameter values $k/M_P$ = 0.01 and 0.2. This updates the results of KHACHATRYAN 16M.

27 SIRUNYAN 18I use 19.7 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 8 TeV to search for narrow resonances decaying to bottom quark pairs. See their Figure 3 for the limit on the KK graviton mass as a function of the cross section times branching fraction in the mass range 325-1200 GeV.

28 AAD 16R use 20.3 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 8 TeV to place a lower bound on the mass of the lightest KK graviton. See their Figure 4 for the limit on the KK graviton mass as a function of the cross section times branching fraction.

29 AAD 15AZ use 20.3 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 8 TeV to place a lower bound on the mass of the lightest KK graviton. See their Figure 2 for limits on the KK graviton mass as a function of the cross section times branching ratio.

30 AAD 15CP use 20.3 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 8 TeV to place a lower bound on the mass of the lightest KK graviton. See their Figures 6b and 6c for the limit on the KK graviton mass as a function of the cross section times branching fraction.

31 AAD 14V use 20.3 (20.5) fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 8 TeV in the dielectron (dimonium) channels to place a lower bound on the mass of the lightest KK graviton. This updates the results of AAD 12CC.

32 AAD 13A use 4.7 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 7 TeV in the $\ell\nu\ell\nu$ channel, to place a lower bound on the mass of the lightest KK graviton.

33 AAD 13AO use 4.7 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 7 TeV in the $\ell\nu\bar{j}\bar{j}$ channel, to place a lower bound on the mass of the lightest KK graviton.

34 AAD 13AS use 4.9 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 7 TeV in the diphoton channel to place lower limits on the mass of the lightest KK graviton. The diphoton channel is combined with previous results in the dielectron and dimonium channels to set the best limit. See their Table 2 for warp parameter values $k/M_P$ between 0.01 and 0.1. This updates the results of AAD 12Y.

35 AAD 12AD use 1.02 fb⁻¹ of data from pp collisions at $\sqrt{s}$ = 7 TeV to search for KK gravitons in a warped extra dimension decaying to $ZZ$ dibosons in the $\ell\bar{\ell}\ell$ and $\ell\bar{\ell}\ell$ channels ($\ell = e, \mu$). The limit is quoted for the combined $\ell\bar{\ell}\ell + \ell\bar{\ell}\ell$ channels. See their Figure 5 for limits on the cross section $\sigma(G \to ZZ)$ as a function of the graviton mass.

36 AALTONEN 12V use 6 fb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s}$ = 1.96 TeV to search for KK gravitons in a warped extra dimension decaying to $ZZ$ dibosons in the $\ell\bar{\ell}\ell$ and $\ell\bar{\ell}\ell$ channels ($\ell = e, \mu$). It provides improved limits over the previous analysis in AALTONEN 11G. See their Figure 16 for limits from all channels combined on the cross section times branching ratio $\sigma(p\bar{p} \to G^+ \to ZZ)$ as a function of the graviton mass.

37 BAAK 12 use electroweak precision observables to place a lower bound on the compactification scale $k e^{-\pi k R}$, assuming Standard Model fields propagate in the bulk and the Higgs is confined to the IR brane. See their Fig. 27 for more details.

38 AALTONEN 11G use 2.5-2.9 fb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s}$ = 1.96 TeV to search for KK gravitons in a warped extra dimension decaying to $ZZ$ dibosons via the $ee\bar{e}, e\mu\mu, \mu\mu\mu, e\bar{e}\bar{e}, \mu\mu\bar{\ell}\bar{\ell}$ channels. See their Fig. 20 for limits on the cross section $\sigma(G \to ZZ)$ as a function of the graviton mass.

39 AALTONEN 11R uses 5.7 fb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s}$ = 1.96 TeV in the dielectron channel to place a lower bound on the mass of the lightest graviton. It provides combined limits with the diphoton channel analysis of AALTONEN 11U. For warp parameter values $k/M_P$ between 0.01 to 0.1 the lower limit on the mass of the lightest graviton is between 612 and 1058 GeV. See their Table I for more details.

40 ABAZOV 11H use 5.4 fb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s}$ = 1.96 TeV to place a lower bound on the mass of the lightest graviton. Their 95% C.L. exclusion limit does not include masses less than 300 GeV.
41 AALTONEN 10n use $2.9 \text{ fb}^{-1}$ of data from $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to place a lower bound on the mass of the lightest graviton.

42 ABAZOV 10F use $5.4 \text{ fb}^{-1}$ of data from $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to place a lower bound on the mass of the lightest graviton. For warp parameter values of $k/M_P$ between 0.01 and 0.1 the lower limit on the mass of the lightest graviton is between 560 and 1050 GeV. See their Fig. 3 for more details.

43 AALTONEN 08S use $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to search for KK gravitons in warped extra dimensions. They search for graviton resonances decaying to four electrons via two Z bosons using $1.1 \text{ fb}^{-1}$ of data. See their Fig. 8 for limits on $\sigma \cdot B(G \rightarrow ZZ)$ versus the graviton mass.

44 ABAZOV 08J use $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to search for KK gravitons in warped extra dimensions. They search for graviton resonances decaying to electrons and photons using $1 \text{ fb}^{-1}$ of data. For warp parameter values of $k/M_P$ between 0.01 and 0.1 the lower limit on the mass of the lightest excitation is between 300 and 900 GeV. See their Fig. 4 for more details.

45 AALTONEN 07G use $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to search for KK gravitons in warped extra dimensions. They search for graviton resonances decaying to photons using $1.2 \text{ fb}^{-1}$ of data. For warp parameter values of $k/M_P = 0.1, 0.05$, and 0.01 the bounds on the graviton mass are 850, 694, and 230 GeV, respectively. See their Fig. 3 for more details. See also AALTONEN 07H.

46 AALTONEN 07H use $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to search for KK gravitons in warped extra dimensions. They search for graviton resonances decaying to electrons using $1.3 \text{ fb}^{-1}$ of data. For a warp parameter value of $k/M_P = 0.1$ the bound on the graviton mass is 807 GeV. See their Fig. 4 for more details. A combined analysis with the diphoton data of AALTONEN 07G yields for $k/M_P = 0.1$ a graviton mass lower bound of 889 GeV.

47 ABAZOV 05N use $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to search for KK gravitons in warped extra dimensions. They search for graviton resonances decaying to muons, electrons or photons, using $260 \text{ pb}^{-1}$ of data. For warp parameter values of $k/M_P = 0.1, 0.05$, and 0.01, the bounds on the graviton mass are 785, 650 and 250 GeV respectively. See their Fig. 3 for more details.

48 ABULENCIA 05A use $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to search for KK gravitons in warped extra dimensions. They search for graviton resonances decaying to muons or electrons, using $200 \text{ pb}^{-1}$ of data. For warp parameter values of $k/M_P = 0.1, 0.05$, and 0.01, the bounds on the graviton mass are 710, 510 and 170 GeV respectively.

### Limits on Kaluza-Klein Gluons in Warped Extra Dimensions

This section places limits on the mass of the first Kaluza-Klein (KK) excitation of the gluon in warped extra dimension models with Standard Model fields propagating in the bulk. Bounds are given for a specific benchmark model with $\Gamma/m = 15.3\%$ where $\Gamma$ is the width and $m$ the mass of the KK gluon. See the "Extra Dimensions" review for more discussion.

<table><thead><tr><th>VALUE (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;3.8</td><td>95</td><td>1 AABOUD</td><td>18BI ATLS</td><td>$g_{KK} \rightarrow t\bar{t} \rightarrow \ell\bar{\ell}$</td></tr><tr><td></td><td></td><td>2 TUMASYAN</td><td>22C CMS</td><td>$g_{KK} \rightarrow Rj \rightarrow jjj$</td></tr><tr><td></td><td></td><td>3 AABOUD</td><td>19AS ATLS</td><td>$g_{KK} \rightarrow t\bar{t} \rightarrow jj$</td></tr><tr><td></td><td></td><td>4 SIRUNYAN</td><td>19AL CMS</td><td>$g_{KK} \rightarrow tT$</td></tr><tr><td>&gt;2.5</td><td>95</td><td>5 CHATRCHYAN</td><td>13BM CMS</td><td>$g_{KK} \rightarrow t\bar{t}$</td></tr><tr><td></td><td></td><td>6 CHEN</td><td>13A</td><td>$B \rightarrow X_S \gamma$</td></tr><tr><td>&gt;1.5</td><td>95</td><td>7 AAD</td><td>12BV ATLS</td><td>$g_{KK} \rightarrow t\bar{t} \rightarrow \ell\bar{\ell}$</td></tr></tbody></table>

1 AABOUD 18BI use $36.1 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV. This result updates AAD 13AQ.

2 TUMASYAN 22C use $138 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to place limits on a KK gluon decaying to gluons via a spin-0 radion, $R$. See their Figure 5 for limits on the cross section times branching fraction as a function of the KK gluon mass and various values of the radion mass.

3 AABOUD 19AS use $36.1 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV. An upper bound of 3.4 TeV is placed on the KK gluon mass for $\Gamma/m = 30\%$.

4 SIRUNYAN 19AL use $35.9 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to place limits on a KK gluon decaying to a top quark and a heavy vector-like fermion, $T$. KK gluon masses between 1.5 and 2.3 TeV and between 2.0 and 2.4 TeV are excluded for T masses of 1.2 and 1.5 TeV, respectively.

5 CHATRCHYAN 13BM use $19.7 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 8$ TeV. Bound is for a width of approximately 15-20% of the KK gluon mass.

6 CHEN 13A place limits on the KK mass scale for a specific warped model with custodial symmetry and bulk fermions. See their Figures 4 and 5.

7 AAD 12BV use $2.05 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 7$ TeV.

### Black Hole Production Limits

<table><thead><tr><th>VALUE (GeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td></td><td>1 SIRUNYAN</td><td>18DA CMS</td><td>$pp \rightarrow \text{multijet}$</td></tr><tr><td></td><td>2 AAD</td><td>16N ATLS</td><td>$pp \rightarrow \text{multijet}$</td></tr><tr><td></td><td>3 AAD</td><td>16O ATLS</td><td>$pp \rightarrow \ell + (\ell\ell/\ell j)/jj$</td></tr><tr><td></td><td>4 AAD</td><td>13AW ATLS</td><td>$pp \rightarrow \mu\mu$</td></tr></tbody></table>

1 SIRUNYAN 18DA use $35.9 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for semiclassical black holes decaying to multijet final states. No excess of events above the expected level of standard model background was observed. Exclusions at 95% CL are set on the mass threshold for black hole production as a function of the higher-dimensional Planck scale for rotating and nonrotating black holes under several model assumptions (ADD, 2, 4, 6 extra dimensions model) in the 7.1-10.3 TeV range. These limits supersede those in SIRUNYAN 17CP.

2 AAD 16N use $3.6 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for semiclassical black hole decays to multijet final states. No excess of events above the expected level of Standard Model background was observed. Exclusion contours at 95% C.L. are set on the mass threshold for black hole production versus higher-dimensional Planck scale for rotating black holes (ADD, 6 extra dimensions model).

3 AAD 16O use $3.2 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for semiclassical black hole decays to high-mass final states with leptons and jets. No excess of events above the expected level of Standard Model background was observed. Exclusion contours at 95% C.L. are set on the mass threshold for black hole production versus higher-dimensional Planck scale for rotating black holes (ADD, 2 to 6 extra dimensions).

4 AAD 13AW use $20.3 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 8$ TeV to search for semiclassical black hole decays to like-sign dimuon final states using large track multiplicity. No excess of events above the expected level of Standard Model background was observed. Exclusion contours at 95% C.L. are set on the mass threshold for black hole production versus higher-dimensional Planck scale in various extra dimensions, rotating and non-rotating models.

<table><caption>Quantum Black Holes</caption><thead><tr><th>VALUE (GeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td></td><td>1 AAD</td><td>23CB ATLS</td><td>$pp \rightarrow e\mu, e\tau, \mu\tau$</td></tr><tr><td></td><td>2 TUMASYAN</td><td>23AW CMS</td><td>$pp \rightarrow \tau\nu$</td></tr><tr><td></td><td>3 TUMASYAN</td><td>23BC CMS</td><td>$pp \rightarrow \gamma j$</td></tr><tr><td></td><td>4 TUMASYAN</td><td>23H CMS</td><td>$pp \rightarrow e\mu, e\tau, \mu\tau$</td></tr><tr><td></td><td>5 AAD</td><td>20T ATLS</td><td>$pp \rightarrow jj$</td></tr><tr><td></td><td>6 AABOUD</td><td>18BA ATLS</td><td>$pp \rightarrow \gamma j$</td></tr><tr><td></td><td>7 SIRUNYAN</td><td>18AT CMS</td><td>$pp \rightarrow e\mu$</td></tr><tr><td></td><td>8 SIRUNYAN</td><td>18DD CMS</td><td>$pp \rightarrow \text{dijet, ang. distrib.}$</td></tr><tr><td></td><td>9 SIRUNYAN</td><td>17CP CMS</td><td>$pp \rightarrow jj$</td></tr><tr><td></td><td>10 KHACHATRY</td><td>16BE CMS</td><td>$pp \rightarrow e\mu$</td></tr><tr><td></td><td>11 KHACHATRY</td><td>15V CMS</td><td>$pp \rightarrow jj$</td></tr><tr><td></td><td>12 AAD</td><td>14AL ATLS</td><td>$pp \rightarrow \ell j$</td></tr><tr><td></td><td>13 AAD</td><td>14V ATLS</td><td>$pp \rightarrow e\epsilon, \mu\mu$</td></tr><tr><td></td><td>14 CHATRCHYAN</td><td>13A CMS</td><td>$pp \rightarrow jj$</td></tr></tbody></table>

1 AAD 23CB use $139 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays with different-flavor high-mass dilepton final states. No excess of events above the expected level of Standard Model background was observed. Exclusion limits at 95% C.L. are set on mass thresholds for black hole production in ADD (6 extra dimensions) and RS1 models. Assuming the black hole mass threshold is equal to the higher-dimensional Planck scale, mass thresholds below 5.9 (3.8), 5.2 (3.0), and 5.1 (3.0) TeV are excluded in the $e\mu, e\tau$ and $\mu\tau$ channels for the ADD (RS1) models, respectively. These limits supersede those in AABOUD 18CM.

2 TUMASYAN 23AW use $138 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays in the tau lepton plus missing transverse momentum final state. Assuming the black hole mass threshold is equal to the higher-dimensional Planck scale, threshold masses below 6.6 TeV are excluded in the ADD model with four extra dimensions (see their Figure 8).

3 TUMASYAN 23BC use $138 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays to final states with a photon and a jet. No excess of events above the expected level of Standard Model background was observed. Exclusion limits at 95% C.L. are set on mass thresholds for black hole production in ADD (6 extra dimensions) and RS1 models. Assuming the black hole mass threshold is equal to the higher-dimensional Planck scale, mass thresholds below 7.5 TeV and 5.2 TeV are excluded for the ADD and RS1 models, respectively (see their Figure 9).

4 TUMASYAN 23H use $138 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays with different-flavor high-mass dilepton final states. No excess of events above the expected level of Standard Model background was observed. Exclusion limits at 95% C.L. are set on mass thresholds for black hole production in the ADD model (with 4 extra dimensions). Assuming the black hole mass threshold is equal to the higher-dimensional Planck scale, mass thresholds below 5.6, 5.2, and 5.0 TeV are excluded in the $e\mu, e\tau$ and $\mu\tau$ channels, respectively.

5 AAD 20T use $139 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays to final states with dijets. No excess of events above the expected level of Standard Model background was observed. Exclusion limits at 95% C.L. are set on mass thresholds for black hole production in an ADD (6 extra dimensions) model. Assuming the black hole mass threshold is equal to the higher-dimensional Planck scale, mass thresholds below 9.4 TeV are excluded. This limit supersedes AABOUD 17AK.

6 AABOUD 18BA use $36.7 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays to final states with a photon and a jet. No excess of events above the expected level of Standard Model background was observed. Exclusion limits at 95% C.L. are set on mass thresholds for black hole production in ADD (6 extra dimensions) and RS1 models. Assuming the black hole mass threshold is equal to the Planck scale, mass thresholds below 7.1 TeV and 4.4 TeV are excluded for the ADD and RS1 models, respectively. These limits supersede those in AAD 16AI.

7 SIRUNYAN 18AT use $35.9 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays to $e\mu$ final states. In Figure 4, lower mass limits of 5.3, 5.5 and 5.6 TeV are placed in a model with 4, 5 and 6 extra dimensions, respectively, and a lower mass limit of 3.6 TeV is found for a single warped dimension.

8 SIRUNYAN 18DD use $35.9 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black hole decays in dijet angular distributions. A lower mass limit of 5.9 (8.2) TeV is placed in the RS (ADD) model with one (six) extra dimension(s).

9 SIRUNYAN 17CP use $2.3 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 13$ TeV to search for quantum black holes decaying to dijet final states. No excess of events above the expected level of standard model background was observed. Limits on the quantum black hole mass threshold are set as a function of the higher-dimensional Planck scale, under the assumption that the mass threshold must exceed the above Planck scale. Depending on the model, mass thresholds in the range up to 5.1-9.0 TeV are excluded.

10 KHACHATRY 16BE use $19.7 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 8$ TeV to search for quantum black holes undergoing lepton flavor violating decay to the $e\mu$ final state. No excess of events above the expected level of standard model background was observed. Exclusion limits at 95% CL are set on mass thresholds for black hole production in the ADD (2-6 flat extra dimensions), RS1 (1 warped extra dimension), and a model with a Planck scale at the TeV scale from a renormalization of the gravitational constant (no extra dimensions). Limits on the black hole mass threshold are set assuming that it is equal to the higher-dimensional Planck scale. Mass thresholds for quantum black holes in the range up to 3.15-3.63 TeV are excluded in the ADD model. In the RS1 model, mass thresholds below 2.81 TeV are excluded in the PDG convention for the Schwarzschild radius. In the model with no extra dimensions, mass thresholds below 1.99 TeV are excluded.

11 KHACHATRY 15V use $19.7 \text{ fb}^{-1}$ of data from $pp$ collisions at $\sqrt{s} = 8$ TeV to search for quantum black holes decaying to dijet final states. No excess of events above
the expected level of standard model background was observed. Exclusion limits at 95% CL are set on mass thresholds for black hole production in the ADD (2–6 flat extra dimensions) and RS1 (1 warped extra dimension) model. Limits on the black hole mass threshold are set as a function of the higher-dimensional Planck scale, under the assumption that the mass threshold must exceed the above Planck scale. Depending on the model, mass thresholds in the range up to 5.0–6.3 TeV are excluded. This paper supersedes CHATRYAN 13AD.

¹² AAD 14A<sub>L</sub> use 20.3 fb⁻¹ of data from *pp* collisions at $\sqrt{s}$ = 8 TeV to search for quantum black hole decays to final states with high-invariant-mass lepton + jet. No excess of events above the expected level of Standard Model background was observed. Exclusion limits at 95% C.L. are set on mass thresholds for black hole production in an ADD (6 extra dimensions) model. Assuming the black hole mass threshold is equal to the higher-dimensional Planck scale, mass thresholds below 3.65 TeV and 2.24 TeV are excluded for the ADD and RS1 models, respectively.

¹³ AAD 14v use 20.3 (20.5) fb⁻¹ of data in the dielectron (dimuon) channels from *pp* collisions at $\sqrt{s}$ = 8 TeV to search for quantum black hole decays involving high-mass dilepton resonances. No excess of events above the expected level of Standard Model background was observed. Exclusion limits at 95% C.L. are set on mass thresholds for black hole production in ADD (6 extra dimensions) and RS1 models. Assuming the black hole mass threshold is equal to the higher-dimensional Planck scale, mass thresholds below 3.65 TeV and 2.24 TeV are excluded for the ADD and RS1 models, respectively.

¹⁴ CHATRYAN 13A<sub>L</sub> use 5 fb⁻¹ of data from *pp* collisions at $\sqrt{s}$ = 7 TeV to search for quantum black holes decaying to dijet final states. No excess of events above the expected level of standard model background was observed. Exclusion limits at 95% CL are set on mass thresholds for black hole production in the ADD (2–6 flat extra dimensions) and RS1 (1 warped extra dimension) model. Limits on the black hole mass thresholds are set as a function of the higher-dimensional Planck scale, under assumption that the mass threshold must exceed the above Planck scale. Depending on the model, mass thresholds in the range up to 4.0–5.3 TeV are excluded.

## REFERENCES FOR Extra Dimensions

<table><thead><tr><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td>AAD</td><td>23CB JHEP 2310 082</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>FLORES</td><td>23 JIMP A38 2350002</td><td>M.M. Flores et al.</td><td>(WITS, WARS, NIP-UPD+)</td></tr><tr><td>TUMASYAN</td><td>23AP JHEP 137813</td><td>A. Tumasyan et al.</td><td>(CMS Coll., B844)</td></tr><tr><td>TUMASYAN</td><td>23AW JHEP 2309 051</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>TUMASYAN</td><td>23BC JHEP 2312 189</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>TUMASYAN</td><td>23H JHEP 2305 227</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AAD</td><td>22F PR D105 092002</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>TUMASYAN</td><td>22D PR B832 137263</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>TUMASYAN</td><td>22D PR D105 032008</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>TUMASYAN</td><td>22J PR D106 012004</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>TUMASYAN</td><td>22R JHEP 2204 087</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>TUMASYAN</td><td>22U JHEP 2205 005</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AAD</td><td>21AF EPJ C81 332</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>21AF B822 136651</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>21F PR D103 112006</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AVNISH</td><td>21 PR D103 115011</td><td>Avnish et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>BLAKEMORE</td><td>21 PR D104 L061101</td><td>C.P. Blakemore et al.</td><td>(STAN)</td></tr><tr><td>HEACOCK</td><td>21 SCI 373 1239</td><td>B. Heacock et al.</td><td>(NIST, RIKEN, NAGO+)</td></tr><tr><td>SIRUNYAN</td><td>21A EPJ C81 13</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>Also</td><td>21N JHEP 2107 208</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>21D JHEP 2111 153</td><td>A. Tumasyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AAD</td><td>20AT EPJ C80 1165</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>20C PL B800 135103</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>20T JHEP 2003 145</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>LEE</td><td>20 PRL 124 011011</td><td>J.G. Lee et al.</td><td>(WASH)</td></tr><tr><td>SIRUNYAN</td><td>20AI JHEP 2005 033</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>20F PR D102 032003</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>20Q EPJ C80 237</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>20A TAN</td><td>20 PRL 124 051301</td><td>W.-H. Tan et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>19A JHEP 190 030</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>19A5 PR D99 092004</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>19A9 PR D94 09024</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>19D JHEP 1909 091</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>Also</td><td>19PL B788 7</td><td>G. Aad et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>19AC JHEP 1904 114</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>19AL EPJ C79 208</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>19BE PRL 122 121803</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>19CF JHEP 1910 125</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AABOUD</td><td>18A1 JHEP 1803 042</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18AL JHEP 1803 009</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18AV JHEP 1807 089</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18BA EPJ C78 102</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18BF EPJ C78 293</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18BI JHEP C78 565</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18CE JHEP 1812 039</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18CJ PR D98 052008</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18CM PR D98 092008</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18CQ PRL 121 191801</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18CW JHEP 1811 040</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18F PL B777 91</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>18I JHEP 1801 126</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>BERGE</td><td>18 PRL 120 141101</td><td>J. Berge et al.</td><td>(MICROSCOPE)</td></tr><tr><td>FAYET</td><td>18 PR D97 055039</td><td>P. Fayet</td><td>(EPOL)</td></tr><tr><td>FAYET</td><td>18A PR D99 055043</td><td>P. Fayet</td><td>(ENSP, EPOL)</td></tr><tr><td>CHDDOCK</td><td>18A PL D97 062002</td><td>C. Haddock et al.</td><td>(NAGO, KE Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18AF PL B781 244</td><td>A.M. Aaboud et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18AS JHEP 1803 003</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18AT JHEP 1804 073</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18AX JHEP 1805 088</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18BX JHEP 1806 120</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18BK JHEP 1807 075</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18BO JHEP 1808 130</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18BV EPJ C78 291</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18CW JHEP 1808 152</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18D1 JHEP 1811 042</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18DD EPJ C78 789</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18DJ JHEP 1809 101</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18D1 PR D98 092001</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18F JHEP 1801 054</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18I PRL 120 201801</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>18S CMS JHEP 092005</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AABOUD</td><td>17AK PR D96 052004</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AABOUD</td><td>17AP PL B775 101</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>KLIMCHITSK...</td><td>17A PR D95 123013</td><td>G.L. Klimchitskaya, V.M. Mostepanenko</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>17AQ JHEP 1710 073</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>SIRUNYAN</td><td>17CP PL B774 279</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AABOUD</td><td>17F JHEP 1707 013</td><td>A.M. Sirunyan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AAD</td><td>16I JHEP 1606 059</td><td>M. Aaboud et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>16AI JHEP 1603 041</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>16N JHEP 1602 026</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>16O PL B760 520</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr></tbody></table>

<table><tbody><tr><td>AAD</td><td>16R PL B755 285</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>KHACHATRY...</td><td>16BE EPJ C76 317</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>KHACHATRY...</td><td>16BQ PR D94 052012</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>KHACHATRY...</td><td>16M PRL 117 051802</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>KHACHATRY...</td><td>16N PL B755 102</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AAD</td><td>15AU JHEP C75 69</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>15AZ JHEP C75 209</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>Also</td><td>15AE JHEP 1504 025</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>15CP JHEP 1512 055</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>15CS PR D91 012008</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>Also</td><td>15D PR D92 059903 (errat.)</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>ACCOMANDO</td><td>15 EJHEP 1540010</td><td>E. Accomando</td><td>(SHMP)</td></tr><tr><td>KHACHATRY...</td><td>15AE JHEP 1504 025</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>KHACHATRY...</td><td>15R PL B749 560</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>KHACHATRY...</td><td>15T PR D91 092005</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>KHACHATRY...</td><td>15V PR D91 052009</td><td>V. Khachatryan et al.</td><td>(CMS Coll.)</td></tr><tr><td>AAD</td><td>14BE EPJ C74 3134</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>14V PR D90 052005</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13A PL B718 860</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13AO PR D87 112006</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13AQ PR D88 012004</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13CJ PRL 143007</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13AW PR D88 072001</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13L PR 110 011802</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13D JHEP 1301 029</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>13E PR D87 015010</td><td>S. Chatrych et al.</td><td>(CMS Coll.)</td></tr><tr><td>CHATRYCH...</td><td>13AD JHEP 1307 178</td><td>S. Chatrych et al.</td><td>(CMS Coll.)</td></tr><tr><td>CHATRYCH...</td><td>13AQ JHEP 078 072005</td><td>S. Chatrych et al.</td><td>(CMS Coll.)</td></tr><tr><td>CHATRYCH...</td><td>13BM PRL 111 211804</td><td>S. Chatrych et al.</td><td>(CMS Coll.)</td></tr><tr><td>Also</td><td>13CH JHEP 119903 (errat.)</td><td>S. Chatrych et al.</td><td>(CMS Coll.)</td></tr><tr><td>CHATRYCH...</td><td>13W PL B718 111</td><td>S. Chatrych et al.</td><td>(CMS Coll.)</td></tr><tr><td>CHEN</td><td>13A CP C37 063102</td><td>J.-B. Chen et al.</td><td>(DALI)</td></tr><tr><td>EDELHAUSER</td><td>13A JHEP 1308 091</td><td>L. Edelhauser, T. Flacke, M. Kramer</td><td>(AACH, KAIST)</td></tr><tr><td>XU</td><td>13 JP G40 035107</td><td>J. Xu et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>12AD PL B712 331</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>12BV JHEP 109 041</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>12CC JHEP 111 138</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>12CP PL B718 411</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>12X PL B710 519</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>12Y PL B710 538</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AALTONEN</td><td>12V PR D85 012008</td><td>T. Aaltonen et al.</td><td>(CDF Coll.)</td></tr><tr><td>ABAZOV</td><td>10F PRL 108 131802</td><td>V.M. Abazov et al.</td><td>(CDF Coll.)</td></tr><tr><td>AJELLO</td><td>12J CJPAC 012 012</td><td>M. Ajello et al.</td><td>(Fermi-LAT Coll.)</td></tr><tr><td>BAAK</td><td>12 EPJ C72 2003</td><td>M. Baak et al.</td><td>(Gifter Group)</td></tr><tr><td>CHATRYCH...</td><td>12R PRL 108 111801</td><td>S. Chatrych et al.</td><td>(CDF Coll.)</td></tr><tr><td>FLACKE</td><td>12 PR D85 126007</td><td>T. Flacke, C. Pasold</td><td>(WURZ)</td></tr><tr><td>NISHIWAKI</td><td>12 PR B707 506</td><td>K. Nishiwaki et al.</td><td>(KOB ESKAK)</td></tr><tr><td>AAD</td><td>11F PRL 106 121803</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AAD</td><td>11X EPJ C71 1744</td><td>G. Aad et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>AALTONEN</td><td>11F PR D83 112008</td><td>T. Aaltonen et al.</td><td>(CDF Coll.)</td></tr><tr><td>AALTONEN</td><td>11R PRL 107 058101</td><td>T. Aaltonen et al.</td><td>(CDF Coll.)</td></tr><tr><td>AALTONEN</td><td>11U PR D83 011102</td><td>T. Aaltonen et al.</td><td>(CDF Coll.)</td></tr><tr><td>AARON</td><td>11C PL B705 52</td><td>F. D. Aaron et al.</td><td>(H1 Coll.)</td></tr><tr><td>ABAZOV</td><td>11H PRL 107 011801</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>BEZZERA</td><td>11I PR D83 075004</td><td>V.B. Bezerra et al.</td><td>(ATLAS Coll.)</td></tr><tr><td>SUSHKOV</td><td>11 PR 107 171011</td><td>A.O. Sushkov et al.</td><td>(CDF Coll.)</td></tr><tr><td>AALTONEN</td><td>10N PR 104 241801</td><td>T. Aaltonen et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABAZOV</td><td>10P PR 104 241802</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABAZOV</td><td>10P PR 105 221802</td><td>V.B. Bezerra et al.</td><td>(D0 Coll.)</td></tr><tr><td>BEZZERA</td><td>10E PR 103 191803</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABAZOV</td><td>09AE PRL 102 051601</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABAZOV</td><td>09D PRL 102 051601</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>MASUDA</td><td>09 PR 102 171101</td><td>M. Masuda, M. Sasaki</td><td>(ICRR)</td></tr><tr><td>AALTONEN</td><td>08AC PRL 101 181602</td><td>T. Aaltonen et al.</td><td>(CDF Coll.)</td></tr><tr><td>08S PR D78 012008</td><td>T. Aaltonen et al.</td><td>T. Aaltonen et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABAZOV</td><td>08J PR 100 091802</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABAZOV</td><td>08S PR 101 011601</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>DAS</td><td>08 PR D78 063011</td><td>P.K. Das, V.H.S. Kumar, P.K. Suresh</td><td>(P.S. Suresh)</td></tr><tr><td>GERACI</td><td>08 PR D78 022002</td><td>A.A. Geraci et al.</td><td>(STAN)</td></tr><tr><td>TRENKEL</td><td>08 PR D77 122001</td><td>C. Trenkel</td><td>(CDF Coll.)</td></tr><tr><td>AALTONEN</td><td>07G PR 99 171801</td><td>T. Aaltonen et al.</td><td>(CDF Coll.)</td></tr><tr><td>AALTONEN</td><td>07H PR 99 171802</td><td>T. Aaltonen et al.</td><td>(CDF Coll.)</td></tr><tr><td>DECCA</td><td>07A EPJ C51 963</td><td>R.S. Decca et al.</td><td>(ALEPH Coll.)</td></tr><tr><td>HAISCH</td><td>07 PR D76 034014</td><td>U. Haisch, A. Weiler</td><td>(DELPHI Coll.)</td></tr><tr><td>KAPNER</td><td>07P PR 98 021101</td><td>D.J. Kapner et al.</td><td>(ALEPH Coll.)</td></tr><tr><td>SCHAEL</td><td>07A EPJ C49 411</td><td>S. Schael et al.</td><td>(ALEPH Coll.)</td></tr><tr><td>TU</td><td>07A PR 98 201101</td><td>L.-C. Tu et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>ABDALLAH</td><td>06C EPJ C45 589</td><td>J. Abdallah et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>ABULENCIA</td><td>06 PR D97 171802</td><td>A. Abulencia et al.</td><td>(CDF Coll.)</td></tr><tr><td>GERDES</td><td>06 PR D73 112008</td><td>D. Gerdes et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>GOGOLADZE</td><td>06 PR D74 093012</td><td>I. Gogoladze, C. Macesanu</td><td>(DELPHI Coll.)</td></tr><tr><td>05N PR D95 091801</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABAZOV</td><td>05V PR 95 161602</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABADALLAH</td><td>05B EPJ C38 395</td><td>J. Abdallah et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>ABULENCIA</td><td>05P PR 95 252001</td><td>A. Abulencia et al.</td><td>(CDF Coll.)</td></tr><tr><td>SMULLIN</td><td>05 PR D72 122001</td><td>S.J. Smullin et al.</td><td>(L3 Coll.)</td></tr><tr><td>ACHARD</td><td>04E PL B587 16</td><td>P. Ahard et al.</td><td>(D0 Coll.)</td></tr><tr><td>ACOSTA</td><td>04C PR 92 121802</td><td>D. Acosta et al.</td><td>(CDF Coll.)</td></tr><tr><td>BARBIERI</td><td>04 NP B703 127</td><td>R. Barbieri et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>CASSE</td><td>04 PL 92 111102</td><td>M. Casse et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>CHEKANOV</td><td>04B PR B591 23</td><td>S. Chekanov et al.</td><td>(ZEUS Coll.)</td></tr><tr><td>HOYLE</td><td>04P PR D70 042004</td><td>C.D. Hoyle et al.</td><td>(WASH)</td></tr><tr><td>ABAZOV</td><td>03 PR 90 251802</td><td>V.M. Abazov et al.</td><td>(D0 Coll.)</td></tr><tr><td>ABENDI</td><td>03D EPJ C26 331</td><td>G. Abendli et al.</td><td>(OPAL Coll.)</td></tr><tr><td>ACHARD</td><td>03D PL B572 133</td><td>P. Ahard et al.</td><td>(L3 Coll.)</td></tr><tr><td>ADLOFF</td><td>03 PL B568 35</td><td>C. Adloff et al.</td><td>(H1 Coll.)</td></tr><tr><td>CHIAVERINI</td><td>03 PL 90 151101</td><td>J. Chilaverini et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>GIUDICE</td><td>03 NP B663 377</td><td>G.F. Giudice, A. Strumia</td><td>(DELPHI Coll.)</td></tr><tr><td>HANNESTAD</td><td>03 PR D67 125008</td><td>S. Hannestad, G.G. Raffelt</td><td>(DELPHI Coll.)</td></tr><tr><td>Also</td><td>03E PL D69 029901 (errat.)</td><td>S. Hannestad, G. Raffelt</td><td>(DELPHI Coll.)</td></tr><tr><td>HEISTER</td><td>03C EPJ C28 1</td><td>A. Heister et al.</td><td>(ALEPH Coll.)</td></tr><tr><td>LONG</td><td>03N NAT 421 922</td><td>J.C. Long et al.</td><td>(L3 Coll.)</td></tr><tr><td>ACHARD</td><td>02 PL B524 65</td><td>P. Ahard et al.</td><td>(L3 Coll.)</td></tr><tr><td>ACHARD</td><td>02D PL B531 28</td><td>P. Ahard et al.</td><td>(L3 Coll.)</td></tr><tr><td>HANNESTAD</td><td>02 PR M8 071301</td><td>S. Hannestad, G. Raffelt</td><td>(DELPHI Coll.)</td></tr><tr><td>ABBOTT</td><td>01 PR M8 1556</td><td>B. Abbott et al.</td><td>(D0 Coll.)</td></tr><tr><td>FAIRBAIRN</td><td>01 PL B508 335</td><td>M. Fairbairn</td><td>(DELPHI Coll.)</td></tr><tr><td>HANHART</td><td>01 PL B509 1</td><td>C. Hanhart et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>HOYLE</td><td>01 PR C6 14818</td><td>C.D. Hoyle et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>ABENDI</td><td>00R EPJ C13 553</td><td>G. Abendli et al.</td><td>(OPAL Coll.)</td></tr><tr><td>ABREU</td><td>00A PR B491 67</td><td>P. Abreu et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>ABREU</td><td>00C PR D61 45</td><td>P. Abreu et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>ABREU</td><td>00Z EPJ C147 53</td><td>P. Abreu et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>CASSI</td><td>00P C481 323</td><td>P. Cassi et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>CHANG</td><td>00B PR M5 3765</td><td>L.N. Chang et al.</td><td>(DELPHI Coll.)</td></tr><tr><td>CHEUNG</td><td>00D PR D61 015005</td><td>K. Cheung</td><td>(DELPHI Coll.)</td></tr><tr><td>CORNET</td><td>00 PR D61 037701</td><td>F. Cornet, M. Relano, J. Rico</td><td>(DELPHI Coll.)</td></tr><tr><td>GRAESSER</td><td>00 PR D61 074019</td><td>M.L. Graesser</td><td>(DELPHI Coll.)</td></tr><tr><td>HAN</td><td>00 PR D62 125018</td><td>T. Han, D. Marfatta, R.-J. Zhang</td><td>(DELPHI Coll.)</td></tr><tr><td>MATHEWS</td><td>00 JHEP 0007 008</td><td>P. Mathews, S. Raychaudhuri, K. Sridhar</td><td>(DELPHI Coll.)</td></tr></tbody></table>
<table><tr><td>MELE</td><td>00</td><td>PR D61 117901</td><td>S. Mele, E. Sanchez</td><td></td></tr><tr><td>RIZZO</td><td>00</td><td>PR D61 016007</td><td>T.G. Rizzo, J.D. Wells</td><td></td></tr><tr><td>ABBIENDI</td><td>99P</td><td>PL B465 303</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ACCIARRI</td><td>99M</td><td>PL B464 135</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>ACCIARRI</td><td>99R</td><td>PL B470 268</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>ACCIARRI</td><td>99S</td><td>PL B470 281</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>BOURILKOV</td><td>99</td><td>JHEP 9908 006</td><td>D. Bourilkov</td><td></td></tr><tr><td>HOSKINS</td><td>85</td><td>PR D32 0384</td><td>J.K. Hoskins et al.</td><td></td></tr></table>

## WIMP and Dark Matter Searches

We omit papers on CHAMP's, millicharged particles, and other exotic particles.

### GALACTIC WIMP SEARCHES

These limits are for weakly-interacting stable particles that may constitute the invisible mass in the galaxy. Unless otherwise noted, a local mass density of 0.3 GeV/cm³ is assumed; see each paper for velocity distribution assumptions. In the papers only the limit is given as a function of the $\chi^0$ mass. Here we list limits only for typical mass values of sub-GeV, GeV, 20 GeV, 100 GeV, and 1 TeV. Specific limits on supersymmetric dark matter particles may be found in the Supersymmetry section.

### Spin-Independent Cross Section Limits for Dark Matter Particle ($\chi^0$) on Nucleon

#### For $m_{\chi^0}$ in GeV range

We provide here limits for $m_{\chi^0} < 5$ GeV

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 3 × 10<sup>-3</sup></td><td>90</td><td>1 AALBERS</td><td>23A</td><td>LZ Si scatter on Xe</td></tr><tr><td>&lt; 4 × 10<sup>-7</sup></td><td>90</td><td>2 AGNES</td><td>23</td><td>DS50 LDM search via Migdal</td></tr><tr><td>&lt; 6 × 10<sup>-7</sup></td><td>90</td><td>3 AGNES</td><td>23B</td><td>DS50 LDM scatter on nucleons</td></tr><tr><td>&lt; 0.5</td><td>90</td><td>4 ALBAKRY</td><td>23</td><td>SCDM LDM via Migdal</td></tr><tr><td>&lt; 1</td><td>95</td><td>5 AMBROSONE</td><td>23</td><td>DM distortion of CR spectra</td></tr><tr><td>&lt;70</td><td>90</td><td>6 ANGLOHER</td><td>23</td><td>CRES LDM search</td></tr><tr><td>&lt; 8 × 10<sup>-8</sup></td><td>90</td><td>7 LI</td><td>23F</td><td>PNDX SI light DM limits</td></tr><tr><td>&lt; 5 × 10<sup>-10</sup></td><td>90</td><td>8 MA</td><td>23A</td><td>PNDX LDM search</td></tr><tr><td>&lt;10</td><td>90</td><td>9 ADHIKARI</td><td>22B</td><td>C100 sub-WIMP via SI coupling/Migdal effect</td></tr><tr><td>&lt; 1.4 × 10<sup>4</sup></td><td>90</td><td>10 ARMENGAUD</td><td>22</td><td>EDEL GeV-scale DM on Ge via Migdal effect</td></tr><tr><td>&lt; 5 × 10<sup>5</sup></td><td>90</td><td>11 CUI</td><td>22</td><td>PNDX sub-GeV boosted DM</td></tr><tr><td>&lt; 6.5 × 10<sup>6</sup></td><td>90</td><td>12 XU</td><td>22</td><td>CDEX sub-GeV DM</td></tr><tr><td>&lt; 2 × 10<sup>-7</sup></td><td>95</td><td>13 AKERIB</td><td>21A</td><td>LUX low mass WIMPs</td></tr><tr><td>&lt; 5 × 10<sup>6</sup></td><td>90</td><td>14 ALKHATIB</td><td>21</td><td>SCDM light DM</td></tr><tr><td>&lt; 1 × 10<sup>8</sup></td><td>95</td><td>15 ANDRIAMIR...</td><td>21A</td><td>sub-GeV DM on nucleon</td></tr><tr><td>&lt; 1 × 10<sup>-8</sup></td><td>90</td><td>16 APRILE</td><td>21</td><td>XEIT GeV scale DM</td></tr><tr><td>&lt; 8 × 10<sup>-4</sup></td><td>90</td><td>17 AGUILAR-AR...</td><td>20C</td><td>DMIC WIMP SI scatter on Si</td></tr><tr><td>&lt; 8 × 10<sup>-4</sup></td><td>90</td><td>18 AKERIB</td><td>20A</td><td>LUX GeV-scale WIMP search</td></tr><tr><td>&lt; 1 × 10<sup>-2</sup></td><td>90</td><td>19 ABDELHAME...</td><td>19A</td><td>CRES CaWO<sub>4</sub></td></tr><tr><td>&lt; 5.4 × 10<sup>-6</sup></td><td>90</td><td>20 AGNESE</td><td>19A</td><td>SCDM light DM on Xe via Migdal/brem effect</td></tr><tr><td>&lt; 1</td><td>90</td><td>21 AKERIB</td><td>19</td><td>LUX GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 1 × 10<sup>-6</sup></td><td>90</td><td>22 AMOLE</td><td>19</td><td>PICO C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 1.6 × 10<sup>-3</sup></td><td>90</td><td>23 APRILE</td><td>19C</td><td>XEIT DM on Xe</td></tr><tr><td>&lt; 1 × 10<sup>-7</sup></td><td>90</td><td>24 APRILE</td><td>19D</td><td>XEIT DM on Xe</td></tr><tr><td>&lt; 0.1</td><td>90</td><td>25 ARMENGAUD</td><td>19</td><td>EDEL GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 1.6 × 10<sup>3</sup></td><td>90</td><td>26 KOBAYASHI</td><td>19</td><td>XMAS annual modulation Xe</td></tr><tr><td>&lt; 7 × 10<sup>2</sup></td><td>90</td><td>27 LIU</td><td>19B</td><td>CDEX Ge; sub-GeV DM via Migdal</td></tr><tr><td>&lt; 7 × 10<sup>-7</sup></td><td>90</td><td>28 AGNES</td><td>18</td><td>DS50 GeV-scale WIMPs on Ar</td></tr><tr><td>&lt; 1.5 × 10<sup>-5</sup></td><td>95</td><td>29 AGNESE</td><td>18</td><td>SCDM GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 2 × 10<sup>-8</sup></td><td>90</td><td>30 APRILE</td><td>18</td><td>XEIT Xe, SI</td></tr><tr><td>&lt; 4.5 × 10<sup>-3</sup></td><td>90</td><td>31 ARNAUD</td><td>18</td><td>NEWS low mass WIMP, Ne</td></tr><tr><td>&lt; 8 × 10<sup>-6</sup></td><td>90</td><td>32 JIANG</td><td>18</td><td>CDEX GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 3 × 10<sup>-5</sup></td><td>90</td><td>33 YANG</td><td>18</td><td>CDEX WIMPs on Ge</td></tr><tr><td>&lt; 1 × 10<sup>-6</sup></td><td>90</td><td>34 AKERIB</td><td>17</td><td>LUX Xe</td></tr><tr><td>&lt; 1 × 10<sup>2</sup></td><td>90</td><td>35 ANGLOHER</td><td>17A</td><td>CRES GeV-scale WIMPs</td></tr><tr><td>&lt; 7 × 10<sup>-5</sup></td><td>90</td><td>36 ANGLOHER</td><td>16</td><td>CRES CaWO<sub>4</sub></td></tr><tr><td>&lt; 3 × 10<sup>-5</sup></td><td>90</td><td>37 APRILE</td><td>16</td><td>X100 Xe</td></tr><tr><td>&lt; 4.3 × 10<sup>-4</sup></td><td>90</td><td>38 ARMENGAUD</td><td>16</td><td>EDE3 GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 7 × 10<sup>-5</sup></td><td>90</td><td>39 HEHN</td><td>16</td><td>EDE3 SI WIMP on Ge</td></tr><tr><td>&lt; 6 × 10<sup>-5</sup></td><td>90</td><td>40 ZHAO</td><td>16</td><td>CDEX GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 1 × 10<sup>-4</sup></td><td>90</td><td>41 AMOLE</td><td>15</td><td>PICO C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 8 × 10<sup>-5</sup></td><td>90</td><td>42 XIAO</td><td>15</td><td>PNDX WIMPs on Xe</td></tr><tr><td>&lt; 3 × 10<sup>-5</sup></td><td>90</td><td>43 AGNESE</td><td>14</td><td>SCDM GeV-scale WIMPs</td></tr><tr><td>&lt; 1 × 10<sup>-3</sup></td><td>90</td><td>44 AKERIB</td><td>14</td><td>LUX WIMP on Xe</td></tr><tr><td>&lt; 9 × 10<sup>-4</sup></td><td>90</td><td>45 LI</td><td>13B</td><td>TEXO WIMPs on Ge</td></tr><tr><td>&lt; 3 × 10<sup>-4</sup></td><td>90</td><td>46 ARCHAMBAU...</td><td>12</td><td>PICA C<sub>4</sub>F<sub>10</sub></td></tr><tr><td>&lt; 2 × 10<sup>-4</sup></td><td>90</td><td>47 AALSETH</td><td>11</td><td>CGNT GeV WIMPs on Ge</td></tr><tr><td>&lt; 5 × 10<sup>-4</sup></td><td>90</td><td>48 AHMED</td><td>11B</td><td>CDM2 GeV-scale WIMPs on Ge</td></tr></tbody></table>

<table><tr><td>&lt; 8 × 10<sup>-5</sup></td><td>90</td><td>49 ANGLE</td><td>11</td><td>XE10 Xe</td></tr><tr><td>&lt; 5 × 10<sup>-4</sup></td><td>90</td><td>50 AKERIB</td><td>10</td><td>CDM2 WIMPs on Ge/Si</td></tr></table>

1. AALBERS 23A search for e recoil events from GeV scale WIMP scatter on Xe. No signal observed. Limits placed on 6 different models including $\sigma^{SI} < 3 \times 10^{-3}$ for $m(\chi) \sim 1$ GeV via Migdal scattering.

2. AGNES 23 for light DM via e recoil/Migdal effect. No signal observed. $\sigma^{SI}(\chi N) < 4 \times 10^{-7}$ pb for $m(\chi) = 3$ GeV.

3. AGNES 23B search for GeV-scale DM scatter on nucleons in Ar. No signal observed. Limit $\sigma^{SI}(\chi N) < 6 \times 10^{-7}$ pb for $m(\chi) = 3$ GeV.

4. ALBAKRY 23 search for light DM via Migdal effect. No signal observed. Allow $\sigma^{SI} < 0.5$ pb for $m(\chi)=1$ GeV (see e.g. Fig. 7).

5. AMBROSONE 23 derive limits on $\sigma(\chi p)$ due to possible DM distortion of cosmic ray spectra as starburst galaxies. Limits placed in $\sigma$ vs. mass ($10^{-3}-10$ MeV) plane, the most stringent given above being at 1 keV.

6. ANGLOHER 23 search for light DM using Si target. No signal observed. Require $\sigma^{SI} < 70$ pb for $m(\chi) = 0.3$ GeV (see e.g. Fig. 5).

7. LI 23F searches for SI light DM scatter from Xe. No signal observed. The quoted limit for $m(\chi) = 4$ GeV.

8. MA 23A search for GeV-scale DM using PandaX-4T. No signal observed. $\sigma(\chi p) < 5 \times 10^{-10}$ pb for $m(\chi) = 10$ GeV.

9. ADHIKARI 22b search for sub-GeV WIMPs via SI and SD detection; no signal detected; limits placed in $m(\chi)$ vs. $\sigma$ plane for $m(\chi): 0.2-3$ GeV; quoted limit is for $m(\chi) = 1$ GeV.

10. ARMENGAUD 22 search for GeV-scale DM scatter on Ge at EDELWEISS via Migdal effect; no signal observed. Limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\text{DM})$ plane; quoted limit is for $m(\text{DM}) = 100$ MeV.

11. CUI 22 search for sub-GeV boosted DM at PandaX-II at CJPL; no signal detected; limits set in $\sigma^{SI}(\chi p)$ vs. $m(\chi)$ plane; quoted limit for $m(\chi) = 0.1$ GeV.

12. XU 22 search for sub-GeV boosted DM in CDEX; no signal observed; limits placed in $\sigma(\chi N)$ vs. $m(\text{DM})$ plane; quoted limit is for $m(\text{DM}) = 0.1$ GeV.

13. AKERIB 21A present new technique for low mass WIMP detection. Require $\sigma^{SI}(\rho_N) < 2 \times 10^{-7}$ pb for m(WIMP) 10 GeV.

14. ALKHATIB 21 search for light DM using SuperCDMS; require $\sigma^{SI}(\rho_N) < 5 \times 10^6$ for $m(\text{DM}) = 0.1$ GeV.

15. ANDRIAMIRADO 21A search for upscattered (boosted) sub-GeV DM interacting with proton in PROSPECT detector. No signal observed. Limits placed in $\sigma(\chi N)$ vs. $m(\text{DM})$ plane for $m(\text{DM}) \sim 1$ keV - 0.5 GeV. The listed limit is for $m(\text{DM}) = 1$ keV.

16. APRILE 21 search for low recoil energy GeV-scale DM in XENON1T with 1.6 keV threshold. No signal in 0.6 t y exposure. Limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\text{DM})$ plane for $m(\text{DM})$ between 3-12 GeV. The listed limit is for $m(\text{DM}) = 5$ GeV.

17. AGUILAR-AREVALO 20C search for WIMP SI scatter on Si using DAMIC at SNOLab; some excess; limits placed in $\sigma$ vs $m(\text{DM})$ for $m(\text{DM})$ in 1.2-10 GeV; quoted limit for m(WIMP) = 2 GeV.

18. AKERIB 20A search for GeV-scale WIMPs via WIMP-nucleon scatter with single photon emission; no signal; limits placed in $m(\text{WIMP})$ vs $\sigma^{SI}$ plane: for example $\sigma^{SI}(\chi n) < 8 \times 10^{-4}$ pb for m(WIMP) = 2.5 GeV.

19. ABDELHAMEED 19A search for GeV scale dark matter SI scatter on CaWO<sub>4</sub>; no signal, limits placed in $\sigma$ vs. mass plane for $m(\text{DM}) \sim 0.1-10$ GeV. The listed limit is for $m(\text{DM}) = 1$ GeV.

20. AGNESE 19A search for 1.5-10 GeV WIMP scatter on Ge in CDMSlite dataset. Limits set in a likelihood analysis. No signal was observed. Limit reported for $m(\chi) = 5$ GeV.

21. AKERIB 19 search for 0.4-5 GeV DM using bremsstrahlung photons and "Migdal" electrons: $1.4 \times 10^4$ kg d exposure of liquid Xe; constraint $\sigma^{SI}(\chi N) < 1$ pb for $m(\chi) = 5$ GeV in light scalar mediator model.

22. AMOLE 19 search for SI WIMP scatter on $C_3F_8$ in PICO-60 bubble chamber; no signal: set limit for spin independent coupling $\sigma^{SI}(\chi N) < 1 \times 10^{-6}$ pb for $m(\chi) = 5$ GeV.

23. APRILE 19c search for light DM scatter on Xe via atomic excitation, ionization (Migdal effect) or bremsstrahlung; no signal, limits placed in $\sigma$ vs. $m(\text{DM})$ plane for $m(\text{DM}) \sim 0.085-2$ GeV. The listed limit is for $m(\text{DM}) = 1$ GeV.

24. APRILE 19d search for light DM scatter on Xe via ionization to probe SI, SD, and $\chi e$ cross sections; with 22 t d exposure, limits placed in various $\sigma$ vs. $m(\text{DM})$ planes. Quoted limit is for $m(\text{DM}) = 5$ GeV.

25. ARMENGAUD 19search for GeV scale WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 0.045-10$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

26. KOBAYASHI 19 search for sub-GeV WIMP annual modulation in Xe via brems; no signal; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m \sim 0.3-1$ GeV; quoted limit is for $m(\chi) = 0.5$ GeV.

27. LIU 19b search for sub-GeV DM using Migdal effect on Ge at CDEX-IB; no signal, require $\sigma^{SI}(\chi N) < 7 \times 10^2$ pb for $m(\chi) = 0.1$ GeV.

28. AGNES 18 search for 1.8-20 GeV WIMP SI scatter on Ar; quoted limit is for $m(\chi) = 5$ GeV.

29. AGNESE 18 search for GeV scale WIMPs using CDMSlite; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m \sim 1.5-20$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

30. APRILE 18 search for WIMP scatter on 1 t yr Xe; no signal, limits set in $\sigma(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 6-1000$ GeV; quoted limit is for $m = 6$ GeV.

31. ARNAUD 18 search for low mass WIMP scatter on Ne via SPC at NEWS-G; limits set in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m \sim 0.5-20$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

32. JIANG 18 search for GeV scale WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 3-10$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

33. YANG 18 search for WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 2-10$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

34. AKERIB 17 search for WIMP scatter on Xe; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 5-1 \times 10^5$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

35. ANGLOHER 17A search for GeV scale WIMP scatter on $Al_2O_3$ crystal; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 0.15-10$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

36. ANGLOHER 16 search for GeV scale WIMP scatter on CaWO<sub>4</sub>; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 0.5-30$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

37. APRILE 16 search for low mass WIMPs via ionization at XENON100; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m \sim 3.5-20$ GeV; quoted limit is for $m(\chi) = 5$ GeV.
38 ARMENGAUD 16 search for GeV scale WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-30 GeV; quoted limit is for m($\chi$) = 5 GeV.

39 HEHN 16 search for low mass WIMPs via SI scatter on Ge target using profile likelihood analysis; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-30 GeV; quoted limit is for m($\chi$) = 5 GeV.

40 ZHAO 16 search for GeV-scale WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-30 GeV; quoted limit is for m($\chi$) = 5 GeV.

41 AMOLE 15 search for WIMP scatter on C$_3$F$_8$ in PICO-2L; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-25 GeV; quoted limit is for m($\chi$) = 5 GeV.

42 XIAO 15 search for WIMP scatter on Xe with PandaX-I; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 5-100 GeV; quoted limit is for m($\chi$) = 5 GeV.

43 AGNESE 14 search for GeV scale WIMPs SI scatter at SuperCDMS; no signal, limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 3.5-30 GeV; quoted limit is for m($\chi$) = 5 GeV.

44 AKERIB 14 search for WIMP scatter on Xe; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 5-5000 GeV. Limit given for m($\chi$) = 5 GeV.

45 LI 13b search for WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-100 GeV; quoted limit is for m($\chi$) = 5 GeV.

46 ARCHAMBAULT 12 search for low mass WIMP scatter on C$_4$F$_10$; limits set in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m ~ 4-12 GeV; quoted limit is for m = 5 GeV.

47 AALSETH 11 search for GeV-scale SI WIMP scatter on Ge; limits placed on $\sigma^{SI}(\chi N)$ for m($\chi$) ~ 3.5-100 GeV; quoted limit is for m($\chi$) = 5 GeV.

48 AHMED 11b search for GeV scale WIMP scatter on Ge in CDMS II; limits placed in $\sigma^{SD}(\chi N)$ vs. m($\chi$) plane for m ~ 4-12 GeV.

49 ANGLE 11 search for GeV scale WIMPs in Xenon-10; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-20 GeV; quoted limit is for m($\chi$) = 5 GeV.

50 AKERIB 10 search for WIMP scatter on Ge/Si in CDMS II; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m ~ 3-100 GeV. Limit given for m(DM) = 5 GeV.

### For $m_{\chi^0} = 20$ GeV

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

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;1 &times; 10<sup>-11</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>SI scatter on Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>2 ABE</td><td>23E XMAS</td><td>WIMP search</td></tr><tr><td>&lt;4 &times; 10<sup>-11</sup></td><td>90</td><td>3 APRILE</td><td>23A XENT</td><td>SI WIMP search</td></tr><tr><td>&lt;5 &times; 10<sup>-11</sup></td><td>90</td><td>4 MENG</td><td>21B PNDX</td><td>Xe WIMP search</td></tr><tr><td>&lt;5 &times; 10<sup>-5</sup></td><td></td><td>5 FELIZARDO</td><td>20 SMPL</td><td>C$_2$ClF$_5$</td></tr><tr><td>&lt;2.2 &times; 10<sup>-10</sup></td><td>90</td><td>6 WANG</td><td>20G PNDX</td><td>Xe TPC</td></tr><tr><td></td><td></td><td>7 ANGLOHER</td><td>19 CRES</td><td>CaWO$_4$</td></tr><tr><td>&lt;7 &times; 10<sup>-5</sup></td><td>90</td><td>8 KIM</td><td>19A KIMS</td><td>Nal</td></tr><tr><td>&lt;3 &times; 10<sup>-7</sup></td><td>90</td><td>9 KOBAYASHI</td><td>19 XMAS</td><td>SI WIMP on Xe</td></tr><tr><td></td><td></td><td>10 SEONG</td><td>19 BELL</td><td>T &rarr; &gamma;A, A &rarr; &chi;&chi;</td></tr><tr><td>&lt;3.5 &times; 10<sup>-5</sup></td><td>90</td><td>11 YANG</td><td>19 CDEX</td><td>annual modulation Ge</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>12 ABE</td><td>18C XMAS</td><td>&chi;O. Xe modulation</td></tr><tr><td>&lt;1.44 &times; 10<sup>-5</sup></td><td>90</td><td>13 ADHIKARI</td><td>18 C100</td><td>Nal</td></tr><tr><td>&lt;3 &times; 10<sup>-7</sup></td><td>90</td><td>14 AGNESE</td><td>18 DS50</td><td>&chi;O-Ar</td></tr><tr><td>&lt;5 &times; 10<sup>-6</sup></td><td>95</td><td>15 AGNESE</td><td>18 SCDM</td><td>Ge</td></tr><tr><td>&lt;4 &times; 10<sup>-8</sup></td><td>90</td><td>16 AGNESE</td><td>18A SCDM</td><td>Ge</td></tr><tr><td>&lt;6 &times; 10<sup>-11</sup></td><td>90</td><td>17 APRILE</td><td>18 XE1T</td><td>Xe, SI</td></tr><tr><td>&lt;4.5 &times; 10<sup>-3</sup></td><td>90</td><td>18 ARNAUD</td><td>18 NEWS</td><td>GeV WIMPs on Ne</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>19 AARTSEN</td><td>17 ICCB</td><td>&nu;, earth</td></tr><tr><td>&lt;2 &times; 10<sup>-10</sup></td><td>90</td><td>20 AKERIB</td><td>17 LUX</td><td>Xe</td></tr><tr><td>&lt;1 &times; 10<sup>-3</sup></td><td>90</td><td>21 BARBOSA-D...17</td><td>17 ICCB</td><td>Nal</td></tr><tr><td>&lt;1.7 &times; 10<sup>-10</sup></td><td>90</td><td>22 CUI</td><td>17A PNDX</td><td>WIMPs on Xe</td></tr><tr><td>&lt;7.3 &times; 10<sup>-7</sup></td><td>90</td><td>AGNES</td><td>16 DS50</td><td>Ar</td></tr><tr><td>&lt;1 &times; 10<sup>-5</sup></td><td>90</td><td>23 AGNESE</td><td>16 CDMS</td><td>Ge</td></tr><tr><td>&lt;2 &times; 10<sup>-4</sup></td><td>90</td><td>24 AGUILAR-AR...16</td><td>16 DICM</td><td>Si CCDs</td></tr><tr><td>&lt;4.5 &times; 10<sup>-5</sup></td><td>90</td><td>25 ANGLOHER</td><td>16 CRES</td><td>CaWO$_4$</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>26 APRILE</td><td>16 X100</td><td>Xe</td></tr><tr><td>&lt;9.4 &times; 10<sup>-8</sup></td><td>90</td><td>27 ARMENGAUD</td><td>16 EDE3</td><td>Ge</td></tr><tr><td>&lt;1.0 &times; 10<sup>-7</sup></td><td>90</td><td>28 HEHN</td><td>16 EDE3</td><td>Ge</td></tr><tr><td>&lt;5 &times; 10<sup>-6</sup></td><td>90</td><td>29 ZHAO</td><td>16 CDEX</td><td>Ge</td></tr><tr><td>&lt;1 &times; 10<sup>-5</sup></td><td>90</td><td>AGNES</td><td>15 DS50</td><td>Ar</td></tr><tr><td>&lt;1.5 &times; 10<sup>-6</sup></td><td>90</td><td>30 AGNESE</td><td>15A CDM2</td><td>Ge</td></tr><tr><td>&lt;1.5 &times; 10<sup>-7</sup></td><td>90</td><td>31 AGNESE</td><td>15B CDM2</td><td>Ge</td></tr><tr><td>&lt;2.0 &times; 10<sup>-7</sup></td><td>90</td><td>32 AMOLE</td><td>15 PICO</td><td>C$_3$F$_8$</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>CHOI</td><td>15 SKAM</td><td>H, solar &nu; (b&ddot;b)</td></tr><tr><td>&lt;1.2 &times; 10<sup>-5</sup></td><td>90</td><td>CHOI</td><td>15 SKAM</td><td>H, solar &nu; (&tau;<sup>+</sup>&tau;<sup>-</sup>)</td></tr><tr><td>&lt;1.19 &times; 10<sup>-6</sup></td><td>90</td><td>33 XIAO</td><td>15 PNDX</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-8</sup></td><td>90</td><td>34 AGNESE</td><td>14 SCDM</td><td>Ge</td></tr><tr><td>&lt;2.0 &times; 10<sup>-7</sup></td><td>90</td><td>35 AGNESE</td><td>14A SCDM</td><td>Ge</td></tr><tr><td>&lt;3.7 &times; 10<sup>-5</sup></td><td>90</td><td>36 AKERIB</td><td>14 LUX</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>37 ANGLOHER</td><td>14 CRES</td><td>CaWO$_4$</td></tr><tr><td>&lt;5 &times; 10<sup>-6</sup></td><td>90</td><td>FELIZARDO</td><td>14 SMPL</td><td>C$_2$ClF$_5$</td></tr><tr><td>&lt;8 &times; 10<sup>-6</sup></td><td>90</td><td>38 LEE</td><td>14A KIMS</td><td>Csl</td></tr><tr><td>&lt;2 &times; 10<sup>-4</sup></td><td>90</td><td>39 LIU</td><td>14A CDEX</td><td>Ge</td></tr><tr><td>&lt;1 &times; 10<sup>-5</sup></td><td>90</td><td>40 YUE</td><td>14 CDEX</td><td>Ge</td></tr><tr><td>&lt;1.08 &times; 10<sup>-4</sup></td><td>90</td><td>41 AARTSEN</td><td>13 ICCB</td><td>H, solar &nu; (&tau;<sup>+</sup>&tau;<sup>-</sup>)</td></tr><tr><td>&lt;1.5 &times; 10<sup>-5</sup></td><td>90</td><td>42 ABE</td><td>13B XMAS</td><td>Xe</td></tr><tr><td>&lt;3.1 &times; 10<sup>-6</sup></td><td>90</td><td>43 AGNESE</td><td>13 CDM2</td><td>Si</td></tr><tr><td>&lt;3.4 &times; 10<sup>-6</sup></td><td>90</td><td>44 AGNESE</td><td>13A CDM2</td><td>Si</td></tr><tr><td>&lt;2.2 &times; 10<sup>-6</sup></td><td>90</td><td>45 AGNESE</td><td>13A CDM2</td><td>Si</td></tr><tr><td>&lt;1.2 &times; 10<sup>-4</sup></td><td>90</td><td>46 BERNABEI</td><td>13A DAMA</td><td>Nal modulation</td></tr><tr><td></td><td></td><td>47 LI</td><td>13B TEXO</td><td>Ge</td></tr></tbody></table>

<table><tbody><tr><td>&lt;1.2 &times; 10<sup>-7</sup></td><td>90</td><td>48 ZHAO</td><td>13 CDEX</td><td>Ge</td></tr><tr><td></td><td></td><td>AKIMOV</td><td>12 ZEP3</td><td>Xe</td></tr><tr><td></td><td></td><td>49 ANGLOHER</td><td>12 CRES</td><td>CaWO<sub>4</sub></td></tr><tr><td>&lt;8 &times; 10<sup>-6</sup></td><td>90</td><td>50 ANGLOHER</td><td>12 CRES</td><td>CaWO<sub>4</sub></td></tr><tr><td>&lt;7 &times; 10<sup>-9</sup></td><td>90</td><td>51 APRILE</td><td>12 X100</td><td>Xe</td></tr><tr><td>&lt;7 &times; 10<sup>-7</sup></td><td>90</td><td>52 ARMENGAUD</td><td>12 EDE2</td><td>Ge</td></tr><tr><td></td><td></td><td>53 BARRETO</td><td>12 DMIC</td><td>CCD</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>BEHNKE</td><td>12 COUP</td><td>CF<sub>3</sub></td></tr><tr><td>&lt;7 &times; 10<sup>-6</sup></td><td>90</td><td>54 FELIZARDO</td><td>12 SMPL</td><td>C<sub>2</sub>ClF<sub>5</sub></td></tr><tr><td>&lt;1.5 &times; 10<sup>-6</sup></td><td>90</td><td>KIM</td><td>12 KIMS</td><td>Csl</td></tr><tr><td>&lt;5 &times; 10<sup>-5</sup></td><td>90</td><td>55 AALSETH</td><td>11 CGNT</td><td>Ge</td></tr><tr><td></td><td></td><td>56 AALSETH</td><td>11A CGNT</td><td>Ge</td></tr><tr><td>&lt;5 &times; 10<sup>-7</sup></td><td>90</td><td>57 AHMED</td><td>11 CDM2</td><td>Ge, inelastic</td></tr><tr><td>&lt;2.7 &times; 10<sup>-7</sup></td><td>90</td><td>58 AHMED</td><td>11A RVUE</td><td>Ge</td></tr><tr><td>&lt;3 &times; 10<sup>-6</sup></td><td>90</td><td>59 ANGLE</td><td>11 XE10</td><td>Xe</td></tr><tr><td>&lt;7 &times; 10<sup>-8</sup></td><td>90</td><td>60 APRILE</td><td>11 X100</td><td>Xe</td></tr><tr><td></td><td></td><td>61 APRILE</td><td>11A X100</td><td>Xe, inelastic</td></tr><tr><td>&lt;2 &times; 10<sup>-8</sup></td><td>90</td><td>51 APRILE</td><td>11B X100</td><td>Xe</td></tr><tr><td></td><td></td><td>62 HORN</td><td>11 ZEP3</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>AHMED</td><td>10 CDM2</td><td>Ge</td></tr><tr><td>&lt;1 &times; 10<sup>-5</sup></td><td>90</td><td>63 AKERIB</td><td>10 CDM2</td><td>Si, Ge, low threshold</td></tr><tr><td>&lt;1 &times; 10<sup>-7</sup></td><td>90</td><td>APRILE</td><td>10 X100</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>ARMENGAUD</td><td>10 EDE2</td><td>Ge</td></tr><tr><td>&lt;4 &times; 10<sup>-5</sup></td><td>90</td><td>FELIZARDO</td><td>10 SMPL</td><td>C<sub>2</sub>ClF<sub>3</sub></td></tr><tr><td>&lt;1.5 &times; 10<sup>-7</sup></td><td>90</td><td>64 AHMED</td><td>09 CDM2</td><td>Ge</td></tr><tr><td>&lt;2 &times; 10<sup>-4</sup></td><td>90</td><td>65 LIN</td><td>09 TEXO</td><td>Ge</td></tr><tr><td></td><td></td><td>66 AALSETH</td><td>08 CGNT</td><td>Ge</td></tr></tbody></table>

1 AALBERS 23 present first limits for WIMP scatter on Xe. $\sigma^{SI}(\chi p) < 1 \times 10^{-11}$ pb for m($\chi$) = 20 GeV.

2 ABE 23E search for WIMP scatter on Xe in XMASS. No signal observed. Require $\sigma^{SI} < 2 \times 10^{-7}$ pb for m($\chi$) = 20 GeV.

3 APRILE 23A present first results from Xe-nton SI WIMP search. No signal observed. Quoted limit is for m($\chi$) = 20 GeV.

4 MENG 21B search for SI WIMP interaction with 3.7 t Xe and 0.63 t yr exposure. No signal observed. Limits placed in m(DM) vs. $\sigma^{SI}$ plane.

5 FELIZARDO 20 presents 2014 SIMPLE bounds on WIMP DM using $C_2ClF_5$ target.

6 WANG 20G search for SI WIMP scatter on Xe with 132 t d exposure of PANDAX-II.

7 ANGLOHER 19 search for low mass WIMP scatter on CaWO$_4$; no signal; limits placed on Wilson coefficients for m($\chi$) = 0.6-60 GeV.

8 KIM 19A search for WIMP scatter in NaI KIMS experiment; no signal: require $\sigma^{SI}(\chi N) < 7 \times 10^{-5}$ pb for m($\chi$) = 20 GeV.

9 KOBAYASHI 19 search for WIMP scatter in XMASS single-phase liquid Xe detector; no signal; require $\sigma^{SI}(\chi N) < 3 \times 10^{-7}$ pb for m($\chi$) = 20 GeV.

10 SEONG 19 search for T → γA, A → χχ via CP-odd Higgs; no signal; limits on BF set; model dependent conversion to WIMP-nucleon scattering cross section limits $\sigma^{SI} < 10^{-36}$ cm$^2$ for m($\chi$) = 0.01-1 GeV.

11 YANG 19 search for low mass wimps via annual modulation in Ge; no signal; require $\sigma^{SI}(\chi N) < 3.5 \times 10^{-5}$ pb for m($\chi$) = 20 GeV.

12 ABE 18C search for WIMP annual modulation signal for m(WIMP): 6-20 GeV; limits set on SI WIMP-nucleon cross section: see Fig. 6.

13 ADHIKARI 18 search for WIMP scatter on NaI; no signal; require $\sigma^{SI} < 1.44 \times 10^{-5}$ pb for m(WIMP) = 20 GeV; inconsistent with DAMA/LIBRA result.

14 AGNES 18 search low mass m(WIMP): 1.8-20 GeV scatter on Ar; limits on SI WIMP-nucleon cross section set in Fig. 8.

15 AGNESE 18 give limits for $\sigma^{SI}(\chi N)$ for m(WIMP) between 1.5 and 20 GeV using CDMSi mode data.

16 AGNESE 18A search for WIMP scatter on Ge at SuperCDMS; 1 event, consistent with expected background; set limit in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m ~ 10-250 GeV.

17 APRILE 18 search for WIMP scatter on 1 t yr Xe; no signal, limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 6-1000 GeV.

18 ARNAUD 18 search for low mass WIMP scatter on Ne via SPC at NEWS-G; limits set in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m ~ 0.5-20 GeV.

19 AARTSEN 17 obtain $\sigma^{SI} < 6 \times 10^{-6}$ pb for m(wimp) = 20 GeV from $\nu$ from earth.

20 AKERIB 17 search for WIMP scatter on Xe; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 5-1 $\times 10^5$ GeV.

21 BARBOSA-DE-SOUZA 17 search for annual modulation of WIMP scatter on NaI 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.

22 CUI 17A search for SI WIMP scatter; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m ~ 10-1 $\times 10^4$ GeV using 54 ton-day exposure of Xe.

23 AGNESE 16 CDMSi excludes low mass WIMPs 1.6-5.5 GeV and SI scattering cross section depending on m(WIMP); see Fig. 4.

24 AGUILAR-AREVALO 16 search low mass 1-10 GeV WIMP scatter on Si CCDs; set limits Fig. 11.

25 ANGLOHER 16 search for GeV scale WIMP scatter on CaWO$_4$; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 0.5-30 GeV.

26 APRILE 16 search for low mass WIMPs via ionization at XENON100; limits placed in $\sigma^{SI}(\chi N)$ vs m($\chi$) plane for m ~ 3.5-20 GeV.

27 ARMENGAUD 16 search for GeV scale WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-30 GeV.

28 HEHN 16 search for low mass WIMPs via SI scatter on Ge target using profile likelihood analysis; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-30 GeV.

29 ZHAO 16 search for GeV-scale WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. m($\chi$) plane for m($\chi$) ~ 4-30 GeV.

30 AGNESE 15A reanalyse AHMED 11B low threshold data. See their Fig. 12 (left) for improved limits extending down to 5 GeV.

31 AGNESE 15B reanalyse AHMED 10 data.
32 See their Fig. 7 for limits extending down to 4 GeV.

33 XIAO 15 search for WIMP scatter on Xe with PandaX-I; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 5-100$ GeV.

34 This limit value is provided by the authors. See their Fig. 4 for limits extending down to $m_{\chi^0} = 3.5$ GeV.

35 This limit value is provided by the authors. AGNESE 14A result is from CDMS/Slite mode operation with enhanced sensitivity to low mass $m_{\chi^0}$. See their Fig. 3 for limits extending down to $m_{\chi^0} = 3.5$ GeV (see also Fig. 4 in AGNESE 14).

36 See their Fig. 5 for limits extending down to $m_{\chi^0} = 5.5$ GeV.

37 See their Fig. 5 for limits extending down to $m_{\chi^0} = 1$ GeV.

38 See their Fig. 5 for limits extending down to $m_{\chi^0} = 5$ GeV.

39 LIU 14A result is based on prototype CDEX-0 detector. See their Fig. 13 for limits extending down to $m_{\chi^0} = 2$ GeV.

40 See their Fig. 4 for limits extending down to $m_{\chi^0} = 4.5$ GeV.

41 AARTSEN 13 search for neutrinos from the Sun arising from the pair annihilation of $\chi^0$ trapped by the sun in data taken between June 2010 and May 2011.

42 See their Fig. 8 for limits extending down to $m_{\chi^0} = 7$ GeV.

43 This limit value is provided by the authors. AGNESE 13 use data taken between Oct. 2006 and July 2007. See their Fig. 4 for limits extending down to $m_{\chi^0} = 7$ GeV.

44 This limit value is provided by the authors. AGNESE 13A use data taken between July 2007 and Sep. 2008. Three candidate events are seen. Assuming these events are real, the best fit parameters are $m_{\chi^0} = 8.6$ GeV and $\sigma = 1.9 \times 10^{-5}$ pb.

45 This limit value is provided by the authors. Limit from combined data of AGNESE 13 and AGNESE 13A. See their Fig. 4 for limits extending down to $m_{\chi^0} = 5.5$ GeV.

46 BERNABEI 13A 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 $\pm$ 0.0012 counts/(day kg keV) with 9.3 sigma C.L. Find period and phase in agreement with expectations from DM particles.

47 Li 13b search for WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 4-100$ GeV.

48 See their Fig. 5 for limits for $m_{\chi^0} = 4-12$ GeV.

49 ANGLOHER 12 observe excess events above the expected background which are consistent with $\chi^0$ with mass $\sim$ 25 GeV (or 12 GeV) and spin-independent $\chi^0$-nucleon cross section of $2 \times 10^{-6}$ pb (or $4 \times 10^{-5}$ pb).

50 Reanalysis of ANGLOHER 09 data with all three nuclides. See also BROWN 12.

51 See also APRILE 14A.

52 See their Fig. 4 for limits extending down to $m_{\chi^0} = 7$ GeV.

53 See their Fig. 13 for cross section limits for $m_{\chi^0}$ between 1.2 and 10 GeV.

54 See also DAHL 12 for a criticism.

55 See their Fig. 4 for limits extending to $m_{\chi^0} = 3.5$ GeV.

56 AALSETH 11A find indications of annual modulation of the data, the energy spectrum being compatible with $\chi^0$ mass around 8 GeV. See also AALSETH 13.

57 AHMED 11 search for $\chi^0$ 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).

58 AHMED 11A combine CDMS II and EDELWEISS data.

59 ANGLE 11 show limits down to $m_{\chi^0} = 4$ GeV on Fig. 3.

60 APRILE 11 reanalyze APRILE 10 data.

61 APRILE 11A search for $\chi^0$ inelastic scattering. See their Fig. 2 and 3 for limits. See also APRILE 14A.

62 HORN 11 perform detector calibration by neutrons. Earlier results are only marginally affected.

63 See their Fig. 10 and 12 for limits extending to $\chi^0$ mass of 1 GeV.

64 Superseded by AHMED 10.

65 See their Fig. 6(a) for cross section limits for $m_{\chi^0}$ extending down to 2 GeV.

66 See their Fig. 2 for cross section limits for $m_{\chi^0}$ between 4 and 10 GeV.

## For $m_{\chi^0} = 100$ GeV

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

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;2.5 &times; 10<sup>-11</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>SI scatter on Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-8</sup></td><td>90</td><td>2 ABE</td><td>23E XMAS</td><td>WIMP search</td></tr><tr><td>&lt;6 &times; 10<sup>-11</sup></td><td>90</td><td>3 APRILE</td><td>23A XENT</td><td>SI WIMP search</td></tr><tr><td>&lt;6 &times; 10<sup>-11</sup></td><td>90</td><td>4 MENG</td><td>21B PNDX</td><td>Xe WIMP search</td></tr><tr><td>&lt;5 &times; 10<sup>-5</sup></td><td></td><td>5 ADHIKARI</td><td>20 DEAP</td><td>Ar</td></tr><tr><td>&lt;4.2 &times; 10<sup>-10</sup></td><td>90</td><td>6 FELIZARDO</td><td>20 SMPL</td><td>W</td></tr><tr><td>&lt;4 &times; 10<sup>-8</sup></td><td>90</td><td>7 WANG</td><td>20G PNDX</td><td>Xe TPC</td></tr><tr><td>&lt;3.9 &times; 10<sup>-9</sup></td><td>90</td><td>8 ABE</td><td>19 XMAS</td><td>Xe</td></tr><tr><td>&lt;2.3 &times; 10<sup>-6</sup></td><td>90</td><td>9 AJAJ</td><td>19 DEAP</td><td>Ar</td></tr><tr><td>&lt;1.14 &times; 10<sup>-8</sup></td><td>90</td><td>10 ADHIKARI</td><td>18 C100</td><td>NaI</td></tr><tr><td>&lt;1.2 &times; 10<sup>-8</sup></td><td>90</td><td>11 AGNES</td><td>18A DS50</td><td>Ar</td></tr><tr><td>&lt;2 &times; 10<sup>-8</sup></td><td>90</td><td>12 AGNESE</td><td>18A CDMS</td><td>Ge</td></tr><tr><td>&lt;1.2 &times; 10<sup>-8</sup></td><td>90</td><td>13 AMAUDRUZ</td><td>18 DEAP</td><td>Ar</td></tr><tr><td>&lt;9.12 &times; 10<sup>-11</sup></td><td>90</td><td>14 APRILE</td><td>18 XE1T</td><td>Xe</td></tr><tr><td>&lt;1.7 &times; 10<sup>-10</sup></td><td>90</td><td>15 REN</td><td>18 PNDX</td><td>SIDM at PDX-II</td></tr><tr><td>&lt;1.2 &times; 10<sup>-10</sup></td><td>90</td><td>16 AKERIB</td><td>17 LUX</td><td>Xe</td></tr><tr><td>&lt;1.2 &times; 10<sup>-10</sup></td><td>90</td><td>17 APRILE</td><td>17G XE1T</td><td>Xe</td></tr><tr><td>&lt;2.0 &times; 10<sup>-8</sup></td><td>90</td><td>18 CUI</td><td>17A PNDX</td><td>Ar</td></tr><tr><td>&lt;1 &times; 10<sup>-9</sup></td><td>90</td><td>AGNES</td><td>16 DS50</td><td>Ar</td></tr><tr><td>&lt;1 &times; 10<sup>-9</sup></td><td>90</td><td>19 AKERIB</td><td>16 LUX</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-8</sup></td><td>90</td><td>20 APRILE</td><td>16B X100</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-8</sup></td><td>90</td><td>21 TAN</td><td>16 PNDX</td><td>Xe</td></tr><tr><td>&lt;6 &times; 10<sup>-8</sup></td><td>90</td><td>22 TAN</td><td>16B Xe</td><td>Xe</td></tr><tr><td>&lt;6 &times; 10<sup>-8</sup></td><td>90</td><td>AGNES</td><td>15 DS50</td><td>Ar</td></tr></tbody></table>

<table><tbody><tr><td>&lt;4 &times; 10<sup>-8</sup></td><td>90</td><td>23 AGNESE</td><td>15B CDM2</td><td>Ge</td></tr><tr><td>&lt;7.13 &times; 10<sup>-6</sup></td><td>90</td><td>CHOI</td><td>15 SKAM</td><td>H, solar &nu; (b<span style="text-decoration: overline">b</span>)</td></tr><tr><td>&lt;6.26 &times; 10<sup>-7</sup></td><td>90</td><td>CHOI</td><td>15 SKAM</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt;2.76 &times; 10<sup>-7</sup></td><td>90</td><td>CHOI</td><td>15 SKAM</td><td>H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td></tr><tr><td>&lt;1.5 &times; 10<sup>-8</sup></td><td>90</td><td>24 XIAO</td><td>15 PNDX</td><td>Xe</td></tr><tr><td>&lt;1 &times; 10<sup>-9</sup></td><td>90</td><td>AKERIB</td><td>14 LUX</td><td>Xe</td></tr><tr><td>&lt;4.0 &times; 10<sup>-6</sup></td><td>90</td><td>25 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt;1.0 &times; 10<sup>-4</sup></td><td>90</td><td>25 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; (b<span style="text-decoration: overline">b</span>)</td></tr><tr><td>&lt;1.6 &times; 10<sup>-6</sup></td><td>90</td><td>25 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td></tr><tr><td>&lt;5 &times; 10<sup>-6</sup></td><td>90</td><td>FELIZARDO</td><td>14 SMPL</td><td>C2CIF<sub>5</sub></td></tr><tr><td>&lt;6.01 &times; 10<sup>-7</sup></td><td>90</td><td>26 AARTSEN</td><td>13 ICCB</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt;3.30 &times; 10<sup>-5</sup></td><td>90</td><td>26 AARTSEN</td><td>13 ICCB</td><td>H, solar &nu; (b<span style="text-decoration: overline">b</span>)</td></tr><tr><td>&lt;1.9 &times; 10<sup>-6</sup></td><td>90</td><td>27 ADRIAN-MAR.13</td><td>14N TR</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt;1.2 &times; 10<sup>-4</sup></td><td>90</td><td>27 ADRIAN-MAR.13</td><td>14N TR</td><td>H, solar &nu; (b<span style="text-decoration: overline">b</span>)</td></tr><tr><td>&lt;7.6 &times; 10<sup>-7</sup></td><td>90</td><td>27 ADRIAN-MAR.13</td><td>14N TR</td><td>H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>28 AGNESE</td><td>13 CDM2</td><td>Si</td></tr><tr><td>&lt;1.6 &times; 10<sup>-6</sup></td><td>90</td><td>29 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt;1.9 &times; 10<sup>-5</sup></td><td>90</td><td>29 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; (b<span style="text-decoration: overline">b</span>)</td></tr><tr><td>&lt;7.1 &times; 10<sup>-7</sup></td><td>90</td><td>29 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td></tr><tr><td>&lt;3.2 &times; 10<sup>-4</sup></td><td>90</td><td>30 LI</td><td>13B</td><td>TEXO WIMPs on Ge</td></tr><tr><td>&lt;1.67 &times; 10<sup>-6</sup></td><td>90</td><td>31 ABBASI</td><td>12 ICCB</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt;1.07 &times; 10<sup>-4</sup></td><td>90</td><td>31 ABBASI</td><td>12 ICCB</td><td>H, solar &nu; (b<span style="text-decoration: overline">b</span>)</td></tr><tr><td>&lt;4 &times; 10<sup>-8</sup></td><td>90</td><td>AKIMOV</td><td>12 ZEP3</td><td>Xe</td></tr><tr><td>&lt;1.4 &times; 10<sup>-6</sup></td><td>90</td><td>32 ANGLOHER</td><td>12 CRES</td><td>CaWO<sub>4</sub></td></tr><tr><td>&lt;3 &times; 10<sup>-9</sup></td><td>90</td><td>33 APRILE</td><td>12 X100</td><td>Xe</td></tr><tr><td>&lt;3 &times; 10<sup>-7</sup></td><td>90</td><td>BEHNKE</td><td>12 COUP</td><td>C3I<sub>3</sub></td></tr><tr><td>&lt;7 &times; 10<sup>-6</sup></td><td>90</td><td>FELIZARDO</td><td>12 SMPL</td><td>C2CIF<sub>5</sub></td></tr><tr><td>&lt;2.5 &times; 10<sup>-7</sup></td><td>90</td><td>34 KIM</td><td>12 KIMS</td><td>Csl</td></tr><tr><td>&lt;2 &times; 10<sup>-4</sup></td><td>90</td><td>AALSETH</td><td>11 CGNT</td><td>Ge</td></tr><tr><td>&lt;3.3 &times; 10<sup>-8</sup></td><td>90</td><td>35 AHMED</td><td>11A</td><td>RVUE Ge</td></tr><tr><td>&lt;3 &times; 10<sup>-8</sup></td><td>90</td><td>37 AJELLO</td><td>11 FLAT</td><td></td></tr><tr><td>&lt;1 &times; 10<sup>-8</sup></td><td>90</td><td>38 APRILE</td><td>11 X100</td><td>Xe</td></tr><tr><td>&lt;5 &times; 10<sup>-8</sup></td><td>90</td><td>39 APRILE</td><td>11A X100</td><td>Xe, inelastic</td></tr><tr><td>&lt;1 &times; 10<sup>-8</sup></td><td>90</td><td>39 APRILE</td><td>11B X100</td><td>Xe</td></tr><tr><td>&lt;4 &times; 10<sup>-8</sup></td><td>90</td><td>40 ARMENGAUD</td><td>11 EDE2</td><td>Ge</td></tr><tr><td>&lt;9 &times; 10<sup>-6</sup></td><td>90</td><td>41 HORN</td><td>11 ZEP3</td><td>Xe</td></tr><tr><td>&lt;5 &times; 10<sup>-8</sup></td><td>90</td><td>AHMED</td><td>10 CDM2</td><td>Ge</td></tr><tr><td>&lt;9 &times; 10<sup>-6</sup></td><td>90</td><td>AKERIB</td><td>10 CDM2</td><td>Si, Ge, low threshold</td></tr><tr><td>&lt;5 &times; 10<sup>-8</sup></td><td>90</td><td>42 AKIMOV</td><td>10 ZEP3</td><td>Xe, inelastic</td></tr><tr><td>&lt;1 &times; 10<sup>-7</sup></td><td>90</td><td>APRILE</td><td>10 X100</td><td>Xe</td></tr><tr><td>&lt;3 &times; 10<sup>-5</sup></td><td>90</td><td>ARMENGAUD</td><td>10 EDE2</td><td>Ge</td></tr><tr><td>&lt;5 &times; 10<sup>-8</sup></td><td>90</td><td>FELIZARDO</td><td>10 SMPL</td><td>C2CIF<sub>3</sub></td></tr><tr><td>&lt;3 &times; 10<sup>-4</sup></td><td>90</td><td>43 AHMED</td><td>09 CDM2</td><td>Ge</td></tr><tr><td>&lt;3 &times; 10<sup>-4</sup></td><td>90</td><td>44 ANGLE</td><td>09 XE10</td><td>Xe, inelastic</td></tr><tr><td>&lt;3 &times; 10<sup>-4</sup></td><td>90</td><td>45 GIULIANI</td><td>09 TEXO</td><td>Ge</td></tr><tr><td>&lt;3 &times; 10<sup>-4</sup></td><td>90</td><td>45 GIULIANI</td><td>09 RVUE</td><td>Ge</td></tr></tbody></table>

1 AALBERS 23 present first LZ limits on SI WIMP-nucleon scatter from Xe. $\sigma^{SI}(\chi p) < 2.5 \times 10^{-11}$ pb for $m(\chi) = 100$ GeV.

2 ABE 23E search for WIMP scatter on Xe in XMASS. No signal observed. Require $\sigma^{SI} < 2 \times 10^{-7}$ pb for $m(\chi) = 100$ GeV.

3 APRILE 23A present first results from Xe-nton SI WIMP search. No signal observed. Quoted limit is for $m(\chi) = 100$ GeV.

4 MENG 21B search for SI WIMP interaction with 3.7 t Xe and 0.63 t yr exposure. No signal observed. Limits placed in m(DM) vs. $\sigma^{SI}$ plane.

5 ADHIKARI 20 search for SI WIMP scatter from Ar in AJAJ 19 data. No signal observed. Limits placed on $\sigma^P$ vs. m(WIMP) for various assumed operators and models.

6 FELIZARDO 20 presents 2014 SIMPLE bounds on WIMP DM using $C_2CIF_5$ target.

7 WANG 20G search for SI WIMP scatter on Xe with 132 t d exposure of PANDAX-II.

8 ABE 19 search for SI DD in single phase Xe; no signal; require $\sigma^{SI}(\chi p) < 4 \times 10^{-8}$ pb for $m(\chi) \sim 100$ GeV.

9 AJAJ 19 search for SI WIMP-nucleon scatter with 758 tonne day exposure of single phase liquid Ar; no signal: require $\sigma^{SI}(\chi N) < 3.9 \times 10^{-9}$ pb for $m(\chi) = 100$ GeV.

10 ADHIKARI 18 search for WIMP scatter on NaI;limit set $\sigma^{SI}(\chi p) < 2.3 \times 10^{-6}$ pb for $m(\chi) = 100$ GeV.

11 AGNES 18A search for WIMP scatter on 46.4 kg Ar; no signal; require $\sigma^{SI}(\chi N) < 1.14 \times 10^{-8}$ pb for $m(\chi) = 100$ GeV.

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

13 AMAUDRUZ 18 search for WIMP scatter on Ar with DEAP-3600; limits set: $\sigma^{SI}(\chi p) < 1.2 \times 10^{-8}$ pb for m(WIMP) = 100 GeV.

14 APRILE 18 search for WIMP scatter on 1.3 t liquid Xe; no signal; require $\sigma^{SI}(\chi p) < 9.12 \times 10^{-11}$ pb for $m(\chi) = 100$ GeV.

15 REN 18 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.

16 AKERIB 17 exclude SI cross section > 1.7 $\times 10^{-10}$ pb for m(WIMP) = 100 GeV. Uses complete LUX data set.

17 APRILE 17g set limit $\sigma^{SI}(\chi p) < 1.2 \times 10^{-10}$ pb for m(WIMP) = 100 GeV using 1 ton fiducial mass Xe TPC. Exposure is 34.2 live days.

18 CUI 17A search for SI WIMP scatter; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m \sim 10^{-1} \times 10^4$ GeV using 54 ton-day exposure of Xe.

19 AKERIB 16 re-analysis of 2013 data exclude SI cross section > $1 \times 10^{-9}$ pb for m(WIMP) = 100 GeV on Xe target.

20 APRILE 16b combined 447 live days using Xe target exclude $\sigma^{SI} > 1.1 \times 10^{-9}$ pb for m(WIMP) = 50 GeV.

21 TAN 16 search for WIMP scatter off Xe target; see SI exclusion plot Fig. 6.

22 TAN 16b search for WIMP-$p$ scatter off Xe target; see Fig. 5 for SI exclusion.
# Searches Particle Listings

## WIMP and Dark Matter Searches

²³AGNESE 15b reanalyse AHMED 10 data.

²⁴XIAO 15 search for WIMP scatter on Xe with PandaX-I; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 5-100$ GeV.

²⁵AVRORIN 14 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken between 1998 and 2003. See their Table 1 for limits assuming annihilation into neutrino pairs.

²⁶AARTSEN 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the sun in data taken between June 2010 and May 2011.

²⁷ADRIAN-MARTINEZ 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the sun in data taken between Jan. 2007 and Dec. 2008.

²⁸AGNESE 13 use data taken between Oct. 2006 and July 2007.

²⁹BOLIEV 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the sun in data taken from 1978 to 2009. See also SUVOROVA 13 for an older analysis of the same data.

³⁰LI 13b search for WIMP scatter on Ge; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 4-100$ GeV.

³¹ABBASI 12 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun. The amount of $X^0$ depends on the $X^0$-proton cross section.

³²Reanalysis of ANGLOHER 09 data with all three nuclides. See also BROWN 12.

³³See also APRILE 14A.

³⁴See their Fig. 6 for a limit on inelastically scattering $X^0$ for $m_{X^0} = 70$ GeV.

³⁵AHMED 11 search for $X^0$ inelastic scattering. See their Fig. 8–10 for limits.

³⁶AHMED 11A combine CDMS and EDELWEISS data.

³⁷AJELLO 11 search for $e^{\pm}$ flux from $X^0$ annihilations in the Sun. Models in which $X^0$ annihilates into an intermediate long-lived weakly interacting particles or $X^0$ scatters inelastically are constrained. See their Fig. 6–8 for limits.

³⁸APRILE 11 reanalyze APRILE 10 data.

³⁹APRILE 11A search for $X^0$ inelastic scattering. See their Fig. 2 and 3 for limits. See also APRILE 14A.

⁴⁰Supersedes ARMENGAUD 10. A limit on inelastic cross section is also given.

⁴¹HORN 11 perform detector calibration by neutrons. Earlier results are only marginally affected.

⁴²AKIMOV 10 give cross section limits for inelastically scattering dark matter. See their Fig. 4.

⁴³Supersedes by AHMED 10.

⁴⁴ANGLE 09 search for $X^0$ inelastic scattering. See their Fig. 4 for limits.

⁴⁵GIULIANI 05 analyzes the spin-independent $X^0$-nucleon cross section limits with both isoscalar and isovector couplings. See their Fig. 3 and 4 for limits on the couplings.

## For $m_{X^0} = 1$ TeV

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

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;2.8 &times; 10<sup>-10</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>SI scatter on Xe</td></tr><tr><td>&lt;1 &times; 10<sup>-7</sup></td><td>90</td><td>2 ABE</td><td>23E XMAS</td><td>WIMP search</td></tr><tr><td>&lt;5 &times; 10<sup>-10</sup></td><td>90</td><td>3 MENG</td><td>21B PNDX</td><td>Xe WIMP search</td></tr><tr><td></td><td></td><td>4 ADHIKARI</td><td>20 DEAP</td><td>Ar</td></tr><tr><td>&lt;4 &times; 10<sup>-9</sup></td><td>90</td><td>5 WANG</td><td>20G PNDX</td><td>Xe TPC</td></tr><tr><td>&lt;3 &times; 10<sup>-6</sup></td><td>90</td><td>6 YAGUNA</td><td>19 Ar</td><td>Ar; I-spin viol DM</td></tr><tr><td>&lt;3.8 &times; 10<sup>-8</sup></td><td>90</td><td>7 AGNES</td><td>18A DS50</td><td>Ar</td></tr><tr><td>&lt;8.24 &times; 10<sup>-10</sup></td><td>90</td><td>8 APRILE</td><td>18 XE1T</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-9</sup></td><td>90</td><td>9 AKERIB</td><td>17 LUX</td><td>Xe</td></tr><tr><td>&lt;0.3</td><td>90</td><td>10 CHEN</td><td>17E PNDX</td><td>&chi;N &rarr; &chi;<sup>*</sup> &rarr; &chi;<sup>γ</sup></td></tr><tr><td>&lt;1.2 &times; 10<sup>-9</sup></td><td>90</td><td>11 CUI</td><td>17A PNDX</td><td>SI WIMPs on Xe</td></tr><tr><td>&lt;8.6 &times; 10<sup>-8</sup></td><td>90</td><td>AGNES</td><td>16 DS50</td><td>Ar</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>AGNES</td><td>15 DS50</td><td>Ar</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>12 AGNESE</td><td>15b CDM2</td><td>Ge</td></tr><tr><td>&lt;1 &times; 10<sup>-8</sup></td><td>90</td><td>AKERIB</td><td>14 LUX</td><td>Xe</td></tr><tr><td>&lt;2.2 &times; 10<sup>-6</sup></td><td>90</td><td>13 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; ($W^{+}W^{-}$)</td></tr><tr><td>&lt;5.5 &times; 10<sup>-5</sup></td><td>90</td><td>13 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; ($b\bar{b}$)</td></tr><tr><td>&lt;6.8 &times; 10<sup>-7</sup></td><td>90</td><td>13 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; ($\tau^{+}\tau^{-}$)</td></tr><tr><td>&lt;3.46 &times; 10<sup>-7</sup></td><td>90</td><td>14 AARTSEN</td><td>13 ICCB</td><td>H, solar &nu; ($W^{+}W^{-}$)</td></tr><tr><td>&lt;7.75 &times; 10<sup>-6</sup></td><td>90</td><td>14 AARTSEN</td><td>13 ICCB</td><td>H, solar &nu; ($b\bar{b}$)</td></tr><tr><td>&lt;6.9 &times; 10<sup>-7</sup></td><td>90</td><td>15 ADRIAN-MAR..13</td><td>ANTR</td><td>H, solar &nu; ($W^{+}W^{-}$)</td></tr><tr><td>&lt;1.5 &times; 10<sup>-5</sup></td><td>90</td><td>15 ADRIAN-MAR..13</td><td>ANTR</td><td>H, solar &nu; ($b\bar{b}$)</td></tr><tr><td>&lt;1.8 &times; 10<sup>-7</sup></td><td>90</td><td>15 ADRIAN-MAR..13</td><td>ANTR</td><td>H, solar &nu; ($\tau^{+}\tau^{-}$)</td></tr><tr><td>&lt;4.3 &times; 10<sup>-6</sup></td><td>90</td><td>16 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; ($W^{+}W^{-}$)</td></tr><tr><td>&lt;3.4 &times; 10<sup>-5</sup></td><td>90</td><td>16 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; ($b\bar{b}$)</td></tr><tr><td>&lt;1.2 &times; 10<sup>-6</sup></td><td>90</td><td>16 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; ($\tau^{+}\tau^{-}$)</td></tr><tr><td>&lt;2.12 &times; 10<sup>-7</sup></td><td>90</td><td>17 ABBASI</td><td>12 ICCB</td><td>H, solar &nu; ($W^{+}W^{-}$)</td></tr><tr><td>&lt;6.56 &times; 10<sup>-6</sup></td><td>90</td><td>17 ABBASI</td><td>12 ICCB</td><td>H, solar &nu; ($b\bar{b}$)</td></tr><tr><td>&lt;4 &times; 10<sup>-7</sup></td><td>90</td><td>AKIMOV</td><td>12 ZEP3</td><td>Xe</td></tr><tr><td>&lt;1.1 &times; 10<sup>-5</sup></td><td>90</td><td>18 ANGLOHER</td><td>12 CRES</td><td>CaWO<sub>4</sub></td></tr><tr><td>&lt;2 &times; 10<sup>-8</sup></td><td>90</td><td>19 APRILE</td><td>12 X100</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-6</sup></td><td>90</td><td>BEHNKE</td><td>12 COUP</td><td>CF<sub>3</sub>I</td></tr><tr><td>&lt;4 &times; 10<sup>-6</sup></td><td>90</td><td>FELIZARDO</td><td>12 SMPL</td><td>C<sub>2</sub>ClF<sub>5</sub></td></tr><tr><td>&lt;1.5 &times; 10<sup>-6</sup></td><td>90</td><td>KIM</td><td>12 KIMS</td><td>CsI</td></tr><tr><td></td><td></td><td>20 AHMED</td><td>11 CDM2</td><td>Ge, inelastic</td></tr><tr><td>&lt;1.5 &times; 10<sup>-7</sup></td><td>90</td><td>21 AHMED</td><td>11A RVUE</td><td>Ge</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>22 APRILE</td><td>11 X100</td><td>Xe</td></tr><tr><td>&lt;8 &times; 10<sup>-8</sup></td><td>90</td><td>19 APRILE</td><td>11b X100</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>23 ARMENGAUD</td><td>11 EDE2</td><td>Ge</td></tr><tr><td></td><td></td><td>24 HORN</td><td>11 ZEP3</td><td>Xe</td></tr><tr><td>&lt;2 &times; 10<sup>-7</sup></td><td>90</td><td>AHMED</td><td>10 CDM2</td><td>Ge</td></tr><tr><td>&lt;4 &times; 10<sup>-7</sup></td><td>90</td><td>APRILE</td><td>10 X100</td><td>Xe</td></tr><tr><td>&lt;6 &times; 10<sup>-7</sup></td><td>90</td><td>ARMENGAUD</td><td>10 EDE2</td><td>Ge</td></tr><tr><td>&lt;3.5 &times; 10<sup>-7</sup></td><td>90</td><td>25 AHMED</td><td>09 CDM2</td><td>Ge</td></tr></tbody></table>

## For Super-heavy dark matter ($m_{X^0} > 10^{10}$ GeV)

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;1 &times; 10<sup>4</sup></td><td>90</td><td>1 ABREU</td><td>23 AUGE</td><td>DM decay to photons</td></tr><tr><td>&lt;2 &times; 10<sup>5</sup></td><td>90</td><td>2 ACEVEDO</td><td>23 DM tracks in ancient mica</td><td></td></tr><tr><td>&lt;9 &times; 10<sup>4</sup></td><td>90</td><td>3 ANGLOHER</td><td>22 CRES</td><td>SD limit using Li</td></tr><tr><td>&lt;40</td><td>90</td><td>4 ANGLOHER</td><td>22A CRES</td><td>SD limit using Li and Al</td></tr><tr><td>&lt;8 &times; 10<sup>4</sup></td><td>90</td><td>5 ABDELHAME..20A</td><td>CRES</td><td>LIAIO<sub>2</sub></td></tr><tr><td>&lt;1 &times; 10<sup>6</sup></td><td>95</td><td>6 ABDELHAME..19</td><td>CRES</td><td>GeV-scale WIMPs on Li</td></tr><tr><td>&lt;3 &times; 10<sup>-4</sup></td><td>90</td><td>7 AMOLE</td><td>19 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt;1.7 &times; 10<sup>4</sup></td><td>90</td><td>8 APRILE</td><td>19C XE1T</td><td>light DM on Xe via<br>Migdal/brem effect</td></tr><tr><td>&lt;8 &times; 10<sup>6</sup></td><td>90</td><td>9 ARMENGAUD</td><td>19 EDEL</td><td>GeV-scale WIMPs on Ge</td></tr><tr><td>&lt;70</td><td>90</td><td>10 XIA</td><td>19A PNDX</td><td>SD WIMP on Xe</td></tr><tr><td>&lt;100</td><td>90</td><td>11 AGNESE</td><td>18 SCDM</td><td>GeV-scale WIMPs on Ge</td></tr><tr><td>&lt;1</td><td>90</td><td>12 AKERIB</td><td>17A LUX</td><td>Xe</td></tr><tr><td>&lt;0.6</td><td>90</td><td>13 FU</td><td>17 PNDX</td><td>SD WIMP on Xe</td></tr><tr><td>&lt;0.2</td><td>90</td><td>14 AMOLE</td><td>15 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt;1.6 &times; 10<sup>-1</sup></td><td>90</td><td>15 ARCHAMBAU..12</td><td>PICA</td><td><sup>19</sup>F</td></tr></tbody></table>

<footnote n="1">¹AALBERS 23 give first LZ limits on WIMP-nucleon scatter from Xe. $\sigma^{SI} < 2.8 \times 10^{-10}$ pb for $m(\chi) = 1$ TeV.</footnote>

<footnote n="2">²ABE 23E search for WIMP scatter on Xe in XMASS. No signal observed. Require $\sigma^{SI} < 2 \times 10^{-7}$ pb for $m(\chi) = 1000$ GeV.</footnote>

<footnote n="3">³MENG 21B search for SI WIMP interaction with 3.7 t Xe and 0.63 t yr exposure. No signal observed. Limits placed in m(DM) vs. $\sigma^{SI}$ plane.</footnote>

<footnote n="4">⁴ADHIKARI 20 search for SI WIMP scatter from Ar in AJAJ 19 data. No signal observed. Limits placed on $\sigma^p$ vs. m(WIMP) for various assumed operators and models.</footnote>

<footnote n="5">⁵WANG 20G search for SI WIMP scatter on Xe with 132 t d exposure of PANDAX-II.</footnote>

<footnote n="6">⁶YAGUNA 19 recasts DEAP-3600 single-phase liquid argon results in limit for isospin violating DM; for $f_n/f_p = -0.69$, requires $\sigma^{SI}(\chi p) < 3 \times 10^{-6}$ pb for $m(\chi) = 1$ TeV.</footnote>

<footnote n="7">⁷AGNES 18A search for WIMP scatter on 46.4 kg Ar; no signal; require $\sigma^{SI}(\chi N) < 3.8 \times 10^{-8}$ pb for $m(\chi) = 1$ TeV.</footnote>

<footnote n="8">⁸APRILE 18 search for WIMP scatter on 1.3 t Xe; no signal seen; require $\sigma^{SI}(\chi p) < 8.24 \times 10^{-10}$ pb for $m(\chi) = 1$ TeV.</footnote>

<footnote n="9">⁹AKERIB 17 search for WIMP scatter on Xe using complete LUX data set; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m(\chi) \sim 5-1 \times 10^5$ GeV.</footnote>

<footnote n="10">¹⁰CHEN 17E search for inelastic WIMP scatter on Xe; require $\sigma^{SI}(\chi N) < 0.3$ pb for $m(\chi) = 1$ TeV and (mass difference) = 300 keV.</footnote>

<footnote n="11">¹¹CUI 17A search for WIMP scatter using 54 ton-day exposure of Xe; limits placed in $\sigma^{SI}(\chi N)$ vs. $m(\chi)$ plane for $m \sim 10^{-1} \times 10^4$ GeV.</footnote>

<footnote n="12">¹²AGNESE 15b reanalyse AHMED 10 data.</footnote>

<footnote n="13">¹³AVRORIN 14 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken between 1998 and 2003. See their Table 1 for limits assuming annihilation into neutrino pairs.</footnote>

<footnote n="14">¹⁴AARTSEN 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken between June 2010 and May 2011.</footnote>

<footnote n="15">¹⁵ADRIAN-MARTINEZ 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken between Jan. 2007 and Dec. 2008.</footnote>

<footnote n="16">¹⁶BOLIEV 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken from 1978 to 2009. See also SUVOROVA 13 for an older analysis of the same data.</footnote>

<footnote n="17">¹⁷ABBASI 12 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun. The amount of $X^0$ depends on the $X^0$-proton cross section.</footnote>

<footnote n="18">¹⁸Reanalysis of ANGLOHER 09 data with all three nuclides. See also BROWN 12.</footnote>

<footnote n="19">¹⁹See also APRILE 14A.</footnote>

<footnote n="20">²⁰AHMED 11 search for $X^0$ inelastic scattering. See their Fig. 8–10 for limits.</footnote>

<footnote n="21">²¹AHMED 11A combine CDMS and EDELWEISS data.</footnote>

<footnote n="22">²²APRILE 11 reanalyze APRILE 10 data.</footnote>

<footnote n="23">²³Supersedes ARMENGAUD 10. A limit on inelastic cross section is also given.</footnote>

<footnote n="24">²⁴HORN 11 perform detector calibration by neutrons. Earlier results are only marginally affected.</footnote>

<footnote n="25">²⁵Supersedes by AHMED 10.</footnote>

<footnote n="1">¹AALBERS 23A search for GeV-scale WIMP scatter on Xe. No signal observed. Limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane. Quoted limit is for $m(\chi) = 1$ GeV via Migdal scattering.</footnote>

<footnote n="2">²ADHIKARI 22b search for sub-GeV WIMPs via SI and SD detection; no signal detected; limits placed in $m(\chi)$ vs. $\sigma$ plane for $m(\chi): 0.2-3$ GeV; quoted limit is for SD $m(\chi) = 1$ GeV.</footnote>

<footnote n="3">³ANGLOHER 22 search for SD WIMP-proton scatter from Li target; no signal detected; limits placed in $\sigma$ vs. m(WIMP) plane; limit quoted for m(WIMP) = 1 GeV.</footnote>

<footnote n="4">⁴ANGLOHER 22A search for spin-dependent DM scatter on Li and Al for m(DM) ~ 0.2-6 GeV; no signal observed; limits set in $\sigma(\chi p)$ vs. m(DM) plane; quoted limit is for m(DM) = 1 GeV.</footnote>

<footnote n="5">⁵ABDELHAMEED 20A use LiAlO₂ target in CRESST to search for SD WIMP scatter on p; no signal; quoted limit is for m(DM) = 1 GeV.</footnote>
⁶ABDELHAMEED 19 search for SD WIMP scatter on $^7$Li; limits placed on $\sigma^{SD}(\chi p)$ for $m(\chi) \sim 0.8-20$ GeV; quoted limit is for $m(\chi) = 1$ GeV.

⁷AMOLE 19 search for SD WIMP scatter on $C_3F_8$ in PICO-60 bubble chamber; no signal: set limit for spin dependent coupling $\sigma^{SD}(\chi p) < 2 \times 10^{-4}$ pb for $m(\chi) = 5$ GeV.

⁸APRILE 19C search for light DM on Xe via Migdal/brem effect; no signal, require $\sigma^{SD}(\chi p) < 1.7 \times 10^4$ pb for $m(\chi) = 1$ GeV.

⁹ARMENGAUD 19 search for GeV scale WIMP scatter on Ge; limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 0.5-10$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

¹⁰XIA 19A search for WIMP scatter on Xe in PandaX-II; limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 5-1 \times 10^5$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

¹¹AGNESE 18 search for GeV scale WIMPs with CDMSlike; limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 1.5-20$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

¹²AKERIB 17A search for SD WIMP scatter on Xe using 129.5 kg yr exposure; limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 6-1 \times 10^5$ GeV.

¹³FU 17 search for SD WIMP scatter on Xe; limits set in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 4-1 \times 10^3$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

¹⁴AMOLE 15 search for WIMP scatter on $C_3F_8$ in PICO-2L; limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 4-1 \times 10^4$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

¹⁵ARCHAMBAULT 12 search for SD WIMP scatter in $^{19}$F with PICASSO; limits set in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m \sim 4-500$ GeV; quoted limit is for $m(\chi) = 5$ GeV.

## For $m_{\chi^0} = 20$ GeV

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

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&middot;&middot;&middot; We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td></tr><tr><td>&lt; 6 &times; 10<sup>-5</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>SD scatter on Xe</td></tr><tr><td>&lt; 3.5 &times; 10<sup>-5</sup></td><td>90</td><td>2 ABBASI</td><td>22B ICCB</td><td>IceCube SD limit</td></tr><tr><td>&lt; 1.5 &times; 10<sup>5</sup></td><td>90</td><td>3 ANGLOHER</td><td>22 CRES</td><td>SD limit using Li</td></tr><tr><td>&lt; 2 &times; 10<sup>-4</sup></td><td>90</td><td>4 HUANG</td><td>22 PNDX</td><td>SD DM limits</td></tr><tr><td>&lt; 9 &times; 10<sup>-5</sup></td><td>90</td><td>5 AARTSEN</td><td>20C ICCB</td><td>SD WIMP on p</td></tr><tr><td>&lt; 2 &times; 10<sup>5</sup></td><td>90</td><td>6 ABDELHAMEED..20A</td><td>CRES LiAlO<sub>2</sub></td><td></td></tr><tr><td>&lt; 5 &times; 10<sup>-3</sup></td><td>90</td><td>7 FELIZARDO</td><td>20 SMPL WIMPS via SIMPLE</td><td></td></tr><tr><td>&lt; 3 &times; 10<sup>5</sup></td><td>95</td><td>8 ABDELHAMEED..19</td><td>CRES 7Li</td><td></td></tr><tr><td>&lt; 2.5 &times; 10<sup>-4</sup></td><td>90</td><td>9 AMOLE</td><td>19 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 2.5 &times; 10<sup>-4</sup></td><td>90</td><td>10 APRILE</td><td>19A XE1T Xe, SD</td><td></td></tr><tr><td>&lt; 1 &times; 10<sup>-3</sup></td><td>90</td><td>11 XIA</td><td>19A PNDX</td><td>SD WIMP on Xe</td></tr><tr><td>&lt; 30</td><td>95</td><td>12 AGNESE</td><td>18 SCDM Ge</td><td></td></tr><tr><td>&lt; 1 &times; 10<sup>-3</sup></td><td>90</td><td>13 AKERIB</td><td>17A LUX</td><td>Xe</td></tr><tr><td>&lt; 1.32 &times; 10<sup>-2</sup></td><td>90</td><td>14 BEHNKE</td><td>17 PICA</td><td>C<sub>4</sub>F<sub>10</sub></td></tr><tr><td>&lt; 2 &times; 10<sup>-3</sup></td><td>90</td><td>15 FU</td><td>17 PNDX</td><td>SD WIMP on Xe</td></tr><tr><td>&lt; 5 &times; 10<sup>-4</sup></td><td>90</td><td>16 AMOLE</td><td>16A PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 2 &times; 10<sup>-6</sup></td><td>90</td><td>17 KHACHATRY..16A</td><td>CMS 8 TeV pp &rarr; Z+E<sub>T</sub>;</td><td>Z &rarr; e&ell;</td></tr><tr><td>&lt; 1.2 &times; 10<sup>-3</sup></td><td>90</td><td>AMOLE</td><td>15 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 1.43 &times; 10<sup>-3</sup></td><td>90</td><td>CHOI</td><td>15 SKAM H, solar &nu; (b&bar;b)</td><td></td></tr><tr><td>&lt; 1.42 &times; 10<sup>-4</sup></td><td>90</td><td>CHOI</td><td>15 SKAM H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td><td></td></tr><tr><td>&lt; 5 &times; 10<sup>-3</sup></td><td>90</td><td>FELIZARDO</td><td>14 SMPL C<sub>2</sub>CIF<sub>5</sub></td><td></td></tr><tr><td>&lt; 1.29 &times; 10<sup>-2</sup></td><td>90</td><td>18 AARTSEN</td><td>13 ICCB H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td><td></td></tr><tr><td>&lt; 3.17 &times; 10<sup>-2</sup></td><td>90</td><td>19 APRILE</td><td>13 X100 Xe</td><td></td></tr><tr><td>&lt; 3 &times; 10<sup>-2</sup></td><td>90</td><td>20 ARCHAMBAU..12</td><td>PICA F (C<sub>4</sub>F<sub>10</sub>)</td><td></td></tr><tr><td>&lt; 6 &times; 10<sup>-2</sup></td><td>90</td><td>BEHNKE</td><td>12 COUP Cf3I</td><td></td></tr><tr><td>&lt; 20</td><td>90</td><td>DAW</td><td>12 DRFT F (CF<sub>4</sub>)</td><td></td></tr><tr><td>&lt; 7 &times; 10<sup>-3</sup></td><td>90</td><td>FELIZARDO</td><td>12 SMPL C<sub>2</sub>CIF<sub>5</sub></td><td></td></tr><tr><td>&lt; 0.15</td><td>90</td><td>KIM</td><td>12 KIMS Csl</td><td></td></tr><tr><td>&lt; 1 &times; 10<sup>5</sup></td><td>90</td><td>21 AHLEN</td><td>11 DMTP F (CF<sub>4</sub>)</td><td></td></tr><tr><td>&lt; 0.1</td><td>90</td><td>21 BEHNKE</td><td>11 COUP Cf3I</td><td></td></tr><tr><td>&lt; 1.5 &times; 10<sup>-2</sup></td><td>90</td><td>22 TANAKA</td><td>11 SKAM H, solar &nu; (b&bar;b)</td><td></td></tr><tr><td>&lt; 0.2</td><td>90</td><td>ARCHAMBAU..09</td><td>PICA F</td><td></td></tr><tr><td>&lt; 4</td><td>90</td><td>LEBEDENKO</td><td>09A ZEP3 Xe</td><td></td></tr><tr><td>&lt; 0.6</td><td>90</td><td>ANGLE</td><td>08A XE10 Xe</td><td></td></tr><tr><td>&lt;100</td><td>90</td><td>ALNER</td><td>07 ZEP2 Xe</td><td></td></tr><tr><td>&lt; 1</td><td>90</td><td>LEE</td><td>07A KIMS Csl</td><td></td></tr><tr><td>&lt; 20</td><td>90</td><td>23 ABBASI</td><td>06 CDMS 73Ge, 29Si</td><td></td></tr><tr><td>&lt; 2</td><td>90</td><td>SHIMIZU</td><td>06A CNTR F (CaF<sub>2</sub>)</td><td></td></tr><tr><td>&lt; 0.5</td><td>90</td><td>ALNER</td><td>05 NAIA NaI</td><td></td></tr><tr><td>&lt; 1.5</td><td>90</td><td>BARNABE-HE..05</td><td>PICA F (C<sub>4</sub>F<sub>10</sub>)</td><td></td></tr><tr><td>&lt; 1.5</td><td>90</td><td>GIRARD</td><td>05 SMPL F (C<sub>2</sub>CIF<sub>5</sub>)</td><td></td></tr><tr><td>&lt; 35</td><td>90</td><td>MIUCHI</td><td>03 BOLO LiF</td><td></td></tr><tr><td>&lt; 30</td><td>90</td><td>TAKEDA</td><td>03 BOLO NaF</td><td></td></tr></tbody></table>

¹AALBERS 23 yield first SD LZ limits on WIMP-p scatter using Xe. $\sigma^{SD}(\chi p) < 6 \times 10^{-5}$ pb for $m(\chi) = 20$ GeV.

²ABBASI 22B search for WIMP annihilation to $b\bar{b}, \tau\bar{\tau}, \nu\bar{\nu}$ in Sun with 7 years data; no signal; limits set in $m(\chi)$ vs. $\sigma^{SD}(\chi p)$ plane for $m(\chi): 10-100$ GeV; quoted limit for $\nu\bar{\nu}$ channel.

³ANGLOHER 22 search for SD WIMP-proton scatter from Li target; no signal detected; limits placed in $\sigma$ vs. m(WIMP) plane.

⁴HUANG 22 search for SD DM scatter on Xe; no signal observed; limits placed in $\sigma(\chi n)$ vs. m(DM) plane; quoted limit is for m(DM) = 20 GeV.

⁵AARTSEN 20C place combined IceCube and Pico-60 velocity-independent limits on spin-dependent WIMP-p scatter $\sigma^{SD}(\chi p) < 9-5$ pb for m(WIMP) = 20 GeV assuming dominant annihilation to $\tau\bar{\tau}$.

⁶ABDELHAMEED 20A use LiAlO₂ target in CRESST to search for spin-dependent WIMP scatter on p; limits set for m(WIMP): 0.3-30 GeV in Fig. 8. Quoted limit is for m(WIMP) = 30 GeV.

⁷FELIZARDO 20 presents 2014 SIMPLE bounds on WIMP DM using $C_2CIF_5$ target.

⁸ABDELHAMEED 19 uses Li₂MoO₄ target to set limit for spin dependent coupling $\sigma^{SD}(\chi p) < 3 \times 10^5$ pb for $m(\chi) = 20$ GeV.

⁹AMOLE 19 search for SD WIMP scatter on $C_3F_8$ in PICO-60 bubble chamber; no signal: set limit for spin dependent coupling $\sigma^{SD}(\chi p) < 2.5 \times 10^{-5}$ pb for $m(\chi) = 20$ GeV.

¹⁰APRILE 19A search for SD WIMP scatter on 1 t yr Xe; no signal, limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m \sim 6-1000$ GeV.

¹¹XIA 19A search for WIMP scatter on Xe in PandaX-II; limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 5-1 \times 10^5$ GeV.

¹²AGNESE 18 give limits for $\sigma^{SD}(p\chi)$ for m(WIMP) between 1.5 and 20 GeV using CDMSlike mode data.

¹³AKERIB 17A search for SD WIMP scatter on Xe using 129.5 kg yr exposure; limits placed in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 6-1 \times 10^5$ GeV.

¹⁴BEHNKE 17 show final Picasso results based on 231.4 kg d exposure at SNOLab for WIMP scatter on $C_4F_{10}$ search via superheated droplet; require $\sigma(\text{SD}) < 1.32 \times 10^{-2}$ pb for m(WIMP) = 20 GeV.

¹⁵FU 17 search for SD WIMP scatter on Xe; limits set in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m(\chi) \sim 4-1 \times 10^3$ GeV.

¹⁶AMOLE 16A require SD WIMP-p scattering < $5 \times 10^{-4}$ pb for m(WIMP) = 20 GeV; bubbles from $C_3F_8$ target.

¹⁷KHACHATRYAN 16A require SD WIMP-p < $2 \times 10^{-6}$ pb for m(WIMP) = 20 GeV from $pp \rightarrow Z + e\bar{\ell}$; $Z \rightarrow e\bar{\ell}$ signal.

¹⁸AARTSEN 13 search for neutrinos from the Sun arising from the pair annihilation of $\chi^0$ trapped by the sun in data taken between June 2010 and May 2011.

¹⁹The value has been provided by the authors. APRILE 13 note that the proton limits on Xe are highly sensitive to the theoretical model used. See also APRILE 14a.

²⁰ARCHAMBAULT 12 search for WIMP scatter on $C_4F_{10}$; limits set in $\sigma^{SD}(\chi p)$ vs. $m(\chi)$ plane for $m \sim 4-500$ GeV.

²¹Use a direction-sensitive detector.

²²TANAKA 11 search for neutrinos from the Sun arising from the pair annihilation of $\chi^0$ trapped by the Sun. The amount of $\chi^0$ depends on the $\chi^0$-proton cross section.

²³See also AKERIB 05.

## For $m_{\chi^0} = 100$ GeV

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

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&middot;&middot;&middot; We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td></tr><tr><td>&lt; 1.5 &times; 10<sup>-4</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>SD scatter on Xe</td></tr><tr><td>&lt; 1</td><td>90</td><td>2 ADHIKARI</td><td>23C C100</td><td>SD WIMP scatter on I</td></tr><tr><td>&lt; 25.7</td><td>90</td><td>3 SHIMADA</td><td>23 NAGE</td><td>directional WIMP search</td></tr><tr><td>&lt; 2.5 &times; 10<sup>-5</sup></td><td>90</td><td>4 ABBASI</td><td>22B ICCB</td><td>IceCube SD limit</td></tr><tr><td>&lt; 2 &times; 10<sup>-4</sup></td><td>90</td><td>5 HUANG</td><td>22 PNDX</td><td>SD DM limits</td></tr><tr><td>&lt; 50</td><td>90</td><td>6 IKEDA</td><td>21 NAGE</td><td>directional gas TPC</td></tr><tr><td>&lt; 3.34 &times; 10<sup>-4</sup></td><td>90</td><td>7 AARTSEN</td><td>20C ICCB</td><td>SD WIMP on p</td></tr><tr><td>&lt; 6.5 &times; 10<sup>-3</sup></td><td>90</td><td>8 FELIZARDO</td><td>20 SMPL</td><td>WIMPS via SIMPLE</td></tr><tr><td>&lt; 4 &times; 10<sup>-5</sup></td><td>90</td><td>9 AMOLE</td><td>19 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 4 &times; 10<sup>-4</sup></td><td>90</td><td>10 APRILE</td><td>19A XE1T Xe, SD</td><td></td></tr><tr><td>&lt; 8 &times; 10<sup>-4</sup></td><td>90</td><td>11 XIA</td><td>19A PNDX</td><td>SD WIMP on Xe</td></tr><tr><td>&lt; 8 &times; 10<sup>-4</sup></td><td>90</td><td>12 AKERIB</td><td>17A LUX</td><td>Xe</td></tr><tr><td>&lt; 5 &times; 10<sup>-5</sup></td><td>90</td><td>13 AMOLE</td><td>17 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 3.3 &times; 10<sup>-2</sup></td><td>90</td><td>14 APRILE</td><td>17A X100</td><td>Xe inelastic</td></tr><tr><td>&lt; 2.8 &times; 10<sup>-1</sup></td><td>90</td><td>15 BATTAT</td><td>17 DRFT</td><td>CS<sub>2</sub></td></tr><tr><td>&lt; 1.5 &times; 10<sup>-3</sup></td><td>90</td><td>16 FU</td><td>17 PNDX</td><td>Xe</td></tr><tr><td>&lt; 0.553-0.019</td><td>95</td><td>17 AABOUD</td><td>16D ATLS</td><td>pp &rarr; j + E<sub>T</sub></td></tr><tr><td>&lt; 1 &times; 10<sup>-5</sup></td><td>90</td><td>18 AABOUD</td><td>16F ATLS</td><td>pp &rarr; &gamma; + E<sub>T</sub></td></tr><tr><td>&lt; 1 &times; 10<sup>-4</sup></td><td>90</td><td>19 AARTSEN</td><td>16C ICCB</td><td>solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt; 2 &times; 10<sup>-4</sup></td><td>90</td><td>20 ADRIAN-MAR..16</td><td>ANTR</td><td>solar &nu; (WW, b&bar;, &tau;&mpir;)</td></tr><tr><td>&lt; 3 &times; 10<sup>-3</sup></td><td>90</td><td>21 AKERIB</td><td>16A LUX</td><td>Xe</td></tr><tr><td>&lt; 5 &times; 10<sup>-4</sup></td><td>90</td><td>22 AMOLE</td><td>16 PICO</td><td>Cf3I</td></tr><tr><td>&lt; 1.5 &times; 10<sup>-3</sup></td><td>90</td><td>AMOLE</td><td>15 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 3.19 &times; 10<sup>-3</sup></td><td>90</td><td>CHOI</td><td>15 SKAM H, solar &nu; (b&bar;b)</td><td></td></tr><tr><td>&lt; 2.80 &times; 10<sup>-4</sup></td><td>90</td><td>CHOI</td><td>15 SKAM H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td><td></td></tr><tr><td>&lt; 1.24 &times; 10<sup>-4</sup></td><td>90</td><td>CHOI</td><td>15 SKAM H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td><td></td></tr><tr><td>&lt; 8 &times; 10<sup>2</sup></td><td>90</td><td>23 NAKAMURA</td><td>15 NAGE</td><td>CF<sub>4</sub></td></tr><tr><td>&lt; 1.7 &times; 10<sup>-3</sup></td><td>90</td><td>24 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt; 4.5 &times; 10<sup>-2</sup></td><td>90</td><td>24 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; (b&bar;b)</td></tr><tr><td>&lt; 7.1 &times; 10<sup>-4</sup></td><td>90</td><td>24 AVRORIN</td><td>14 BAIK</td><td>H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td></tr><tr><td>&lt; 6 &times; 10<sup>-3</sup></td><td>90</td><td>FELIZARDO</td><td>14 SMPL</td><td>C<sub>2</sub>CIF<sub>5</sub></td></tr><tr><td>&lt; 2.68 &times; 10<sup>-4</sup></td><td>90</td><td>25 AARTSEN</td><td>13 ICCB</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt; 1.47 &times; 10<sup>-2</sup></td><td>90</td><td>25 AARTSEN</td><td>13 ICCB</td><td>H, solar &nu; (b&bar;b)</td></tr><tr><td>&lt; 8.5 &times; 10<sup>-4</sup></td><td>90</td><td>26 ADRIAN-MAR..13</td><td>ANTR</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt; 5.5 &times; 10<sup>-2</sup></td><td>90</td><td>26 ADRIAN-MAR..13</td><td>ANTR</td><td>H, solar &nu; (b&bar;b)</td></tr><tr><td>&lt; 3.4 &times; 10<sup>-4</sup></td><td>90</td><td>26 ADRIAN-MAR..13</td><td>ANTR</td><td>H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td></tr><tr><td>&lt; 1.00 &times; 10<sup>-2</sup></td><td>90</td><td>27 APRILE</td><td>13 X100</td><td>Xe</td></tr><tr><td>&lt; 7.1 &times; 10<sup>-4</sup></td><td>90</td><td>28 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt; 8.4 &times; 10<sup>-3</sup></td><td>90</td><td>28 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; (b&bar;b)</td></tr><tr><td>&lt; 3.1 &times; 10<sup>-4</sup></td><td>90</td><td>28 BOLIEV</td><td>13 BAKS</td><td>H, solar &nu; (&tau;<sup>+</sup> &tau;<sup>-</sup>)</td></tr><tr><td>&lt; 7.07 &times; 10<sup>-4</sup></td><td>90</td><td>29 ABBASI</td><td>12 ICCB</td><td>H, solar &nu; (W<sup>+</sup> W<sup>-</sup>)</td></tr><tr><td>&lt; 4.53 &times; 10<sup>-2</sup></td><td>90</td><td>29 ABBASI</td><td>12 ICCB</td><td>H, solar &nu; (b&bar;b)</td></tr><tr><td>&lt; 7 &times; 10<sup>-2</sup></td><td>90</td><td>30 ARCHAMBAU..12</td><td>PICA</td><td>F (C<sub>4</sub>F<sub>10</sub>)</td></tr><tr><td>&lt; 1 &times; 10<sup>-2</sup></td><td>90</td><td>BEHNKE</td><td>12 COUP</td><td>Cf3I</td></tr><tr><td>&lt; 1.8</td><td>90</td><td>DAW</td><td>12 DRFT</td><td>F (CF<sub>4</sub>)</td></tr><tr><td>&lt; 9 &times; 10<sup>-3</sup></td><td>90</td><td>FELIZARDO</td><td>12 SMPL</td><td>C<sub>2</sub>CIF<sub>5</sub></td></tr><tr><td>&lt; 2 &times; 10<sup>-2</sup></td><td>90</td><td>KIM</td><td>12 KIMS</td><td>Csl</td></tr><tr><td>&lt; 2 &times; 10<sup>3</sup></td><td>90</td><td>23 AHLEN</td><td>11 DMTP</td><td>F (CF<sub>4</sub>)</td></tr></tbody></table>
# Searches Particle Listings

## WIMP and Dark Matter Searches

<table><tr><td>&lt; 7 &times; 10<sup>-2</sup></td><td>90</td><td>BEHNKE</td><td>11</td><td>COUP CF<sub>3</sub>l</td></tr><tr><td>&lt; 2.7 &times; 10<sup>-4</sup></td><td>90</td><td>31 TANAKA</td><td>11</td><td>SKAM H, solar &nu; (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 4.5 &times; 10<sup>-3</sup></td><td>90</td><td>31 TANAKA</td><td>11</td><td>SKAM H, solar &nu; (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 6 &times; 10<sup>3</sup></td><td>90</td><td>32 FELIZARDO</td><td>10</td><td>SMPL C<sub>2</sub>ClF<sub>3</sub></td></tr><tr><td>&lt; 0.4</td><td>90</td><td>23 MIUCHI</td><td>10</td><td>NAGE CF<sub>4</sub></td></tr><tr><td>&lt; 0.8</td><td>90</td><td>ARCHAMBAU.,09</td><td>09A</td><td>PICA F</td></tr><tr><td>&lt; 1.0</td><td>90</td><td>LEBEDENKO</td><td>09A</td><td>ZEP3 Xe</td></tr><tr><td>&lt; 15</td><td>90</td><td>ALNER</td><td>07</td><td>ZEP2 Xe</td></tr><tr><td>&lt; 0.2</td><td>90</td><td>LEE</td><td>07A</td><td>KIMS Csl</td></tr><tr><td>&lt; 1 &times; 10<sup>4</sup></td><td>90</td><td>23 MIUCHI</td><td>07</td><td>NAGE F (CF<sub>4</sub>)</td></tr><tr><td>&lt; 5</td><td>90</td><td>33 AKERIB</td><td>06</td><td>CDMS 73<sub>Ge</sub>, 29<sub>Si</sub></td></tr><tr><td>&lt; 2</td><td>90</td><td>SHIMIZU</td><td>06A</td><td>CNTR F (CaF<sub>2</sub>)</td></tr><tr><td>&lt; 0.3</td><td>90</td><td>ALNER</td><td>05</td><td>NAIA NaI</td></tr><tr><td>&lt; 2</td><td>90</td><td>BARNABE-HE.,05</td><td>05A</td><td>PICA F (C<sub>4</sub>F<sub>10</sub>)</td></tr><tr><td>&lt;100</td><td>90</td><td>BENOIT</td><td>05</td><td>EDEL 73<sub>Ge</sub></td></tr><tr><td>&lt; 1.5</td><td>90</td><td>GIRARD</td><td>05</td><td>SMPL F (C<sub>2</sub>ClF<sub>5</sub>)</td></tr><tr><td>&lt; 0.7</td><td></td><td>34 GIULIANI</td><td>05A</td><td>RVUE</td></tr><tr><td></td><td></td><td>35 GIULIANI</td><td>04</td><td>RVUE</td></tr><tr><td></td><td></td><td>36 GIULIANI</td><td>04A</td><td>RVUE</td></tr><tr><td>&lt; 35</td><td>90</td><td>MIUCHI</td><td>03</td><td>BOLO LiF</td></tr><tr><td>&lt; 40</td><td>90</td><td>TAKEDA</td><td>03</td><td>BOLO NaF</td></tr></table>

1 AALBERS 23 yield first SD LZ limits on WIMP-p scatter using Xe. $\sigma^{SD}(\chi p) < 1.5 \times 10^{-4}$ pb for m(χ) = 100 GeV.

2 ADHIKARI 23c search for SD WIMP scatter on I. No signal observed. Require $\sigma^{SD}(\chi p) < 1$ pb for m(χ) = 100 GeV.

3 SHIMADA 23 search for WIMPs in NEWAGE directional detector. No signal observed. Limits placed in $\sigma^{SD}(\chi p)$ vs. mass. Quoted limit for m(χ) = 150 GeV.

4 ABBASI 22b search for WIMP annihilation to $b\bar{b}\tau\tau$, $\nu\bar{\nu}\tau$ in Sun with 7 years data; no signal; limits set in m(χ) vs. $\sigma^{SD}(\chi p)$ plane for m(χ): 10–100 GeV; quoted limit for $\nu\bar{\nu}\tau$ channel.

5 HUANG 22 search for SD DM scatter on Xe; no signal observed; limits placed in $\sigma(\chi n)$ vs. m(DM) plane; quoted limit is for m(DM) = 100 GeV.

6 IKEDA 21 use direction sensitive TPC NEWAGE to search for SD WIMPs. No signal observed. Limits set in $\sigma^{SD}(\chi p)$ vs. m plane; $\sigma^{SD}(\chi p) < 50$ pb for m(DM) = 100 GeV.

7 AARTSEN 20c place combined IceCube and Pico-60 velocity-independent limits on spin-dependent WIMP-p scatter $\sigma^{SD}(\chi p) < 3.34 \times 10^{-4}$ pb for m(WIMP) = 100 GeV assuming dominant annihilation to $\tau\bar{\tau}$.

8 FELIZARDO 20 presents 2014 SIMPLE bounds on WIMP DM using $C_2ClF_5$ target.

9 AMOLE 19 search for SD WIMP scatter on $C_3F_8$ in PICO-60 bubble chamber; no signal: set limit for spin dependent coupling $\sigma^{SD}(\chi p) < 4 \times 10^{-5}$ pb for m(χ) = 100 GeV.

10 APRILE 19a search for SD WIMP scatter on 1 t yr Xe; no signal, limits placed in $\sigma^{SD}(\chi p)$ vs. m(χ) plane for m ~ 6–1000 GeV.

11 XIA 19a search for WIMP scatter on Xe in Panda-II; limits placed in $\sigma^{SD}(\chi p)$ vs. m(χ) plane for m(χ) ~ 5–1 × 10⁵ GeV.

12 AKERIB 17a search for SD WIMP scatter on Xe using 129.5 kg yr exposure; limits placed in $\sigma^{SD}(\chi p)$ vs. m(χ) plane for m(χ) ~ 6–1 × 10⁵ GeV.

13 AMOLE 17 require $\sigma(\text{WIMP-p})^{SD} < 5 \times 10^{-5}$ pb for m(WIMP) = 100 GeV using PICO-60 1167 kg-days exposure at SNOLab.

14 APRILE 17a require $\sigma(\text{WIMP-p})(\text{inelastic})^{SD} < 3.3 \times 10^{-2}$ pb for m(WIMP) = 100 GeV, based on 7640 kg day exposure at LNGS.

15 BATTAT 17 use directional detection of $C_2$ ions to require $\sigma(\text{SD}) < 2.8 \times 10^{-1}$ pb for 100 GeV WIMP with a 55 days exposure at the Boulby Underground Science Facility.

16 FU 17 from a 33000 kg exposure at CJPL, PANDAX II derive for m(DM) = 100 GeV, $\sigma^{SD}(\text{WIMP-p}) < 2 \times 10^{-3}$ pb.

17 AABOUD 16d use ATLAS 13 TeV 3.2 fb⁻¹ of data to search for monojet plus missing $E_T$; agree with SM rates; present limits on large extra dimensions, compressed SUSY spectra and wimp pair production.

18 AABOUD 16f search for monophoton plus missing $E_T$ events at ATLAS with 13 TeV and 3.2 fb⁻¹; signal agrees with SM background; place limits on SD WIMP-proton scattering vs. mediator mass and large extra dimension models.

19 AARTSEN 16c search for high energy $\nu s$ from WIMP annihilation in solar core; limits set on SD WIMP-p scattering (Fig. 8).

20 ADRIAN-MARTINEZ 16 search for WIMP annihilation into $\nu s$ from solar core; exclude SD cross section < few $10^{-4}$ depending on m(WIMP).

21 AKERIB 16a using 2013 data exclude SD WIMP-proton scattering > 3 × 10⁻³ pb for m(WIMP) = 100 GeV.

22 AMOLE 16 use bubble technique on $C_3F_3$ target to exclude SD WIMP-p scattering > 5 × 10⁻⁴ pb for m(WIMP) = 100 GeV.

23 Use a direction-sensitive detector.

24 AVRIN 14 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken between 1998 and 2003. See their Table 1 for limits assuming annihilation into neutrino pairs.

25 AARTSEN 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken between June 2010 and May 2011.

26 ADRIAN-MARTINEZ 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken between Jan. 2007 and Dec. 2008.

27 The value has been provided by the authors. APRILE 13 note that the proton limits on Xe are highly sensitive to the theoretical model used. See also APRILE 14a.

28 BOLIEV 13 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun in data taken from 1978 to 2009. See also SUVOROVA 13 for an older analysis of the same data.

29 ABBASI 12 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun. The amount of $X^0$ depends on the $X^0$-proton cross section.

30 ARCHAMBAULT 12 search for WIMP scatter on $C_4F_{10}$; limits set in $\sigma^{SD}(\chi p)$ vs. m(χ) plane for m ~ 4–500 GeV.

31 TANAKA 11 search for neutrinos from the Sun arising from the pair annihilation of $X^0$ trapped by the Sun. The amount of $X^0$ depends on the $X^0$-proton cross section.

32 See their Fig. 3 for limits on spin-dependent proton couplings for $X^0$ mass of 50 GeV.

33 See also AKERIB 05.

34 GIULIANI 05A analyze available data and give combined limits.

35 GIULIANI 04 reanalyze COLLAR 00 data and give limits for spin-dependent $X^0$-proton coupling.

36 GIULIANI 04A give limits for spin-dependent $X^0$-proton couplings from existing data.

### For $m_{X^0} = 1$ TeV

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

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 1.5 &times; 10<sup>-3</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>SD scatter on Xe</td></tr><tr><td>&lt; 0.2</td><td>90</td><td>2 ADHIKARI</td><td>23c C100</td><td>SD WIMP scatter on I</td></tr><tr><td>&lt; 1.2 &times; 10<sup>-3</sup></td><td>90</td><td>3 HUANG</td><td>22 PNDX</td><td>SD DM limits</td></tr><tr><td>&lt;200</td><td>90</td><td>4 IKEDA</td><td>21 NAGE</td><td>directional gas TPC</td></tr><tr><td>&lt; 4.81 &times; 10<sup>-3</sup></td><td>90</td><td>5 AARTSEN</td><td>20c ICCB</td><td>SD WIMP on p</td></tr><tr><td>&lt; 3 &times; 10<sup>-4</sup></td><td>90</td><td>6 AMOLE</td><td>19 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 4 &times; 10<sup>-3</sup></td><td>90</td><td>7 APRILE</td><td>19a XE1T</td><td>Xe, SD</td></tr><tr><td>&lt; 5 &times; 10<sup>-3</sup></td><td>90</td><td>8 XIA</td><td>19a PNDX</td><td>SD WIMP on Xe</td></tr><tr><td></td><td></td><td>9 ALBERT</td><td>18c HAWC</td><td>DM annihilation in Sun to long-lived mediator</td></tr><tr><td>&lt; 2.05 &times; 10<sup>-5</sup></td><td>90</td><td>10 AARTSEN</td><td>17a ICCB</td><td>$\nu$, sun</td></tr><tr><td>&lt; 7 &times; 10<sup>-3</sup></td><td>90</td><td>11 AKERIB</td><td>17a LUX</td><td>Xe</td></tr><tr><td>&lt; 2 &times; 10<sup>-2</sup></td><td>90</td><td>12 FU</td><td>17 PNDX</td><td>SD WIMP on Xe</td></tr><tr><td>&lt; 1 &times; 10<sup>-2</sup></td><td>90</td><td>13 ADRIAN-MAR.16b</td><td>ANTR</td><td>solar $\mu$ from WIMP annih.</td></tr><tr><td>&lt; 1.5 &times; 10<sup>3</sup></td><td>90</td><td>AMOLE</td><td>15 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 2.7 &times; 10<sup>-3</sup></td><td>90</td><td>NAKAMURA</td><td>15 NAGE</td><td>CF<sub>4</sub></td></tr><tr><td>&lt; 6.9 &times; 10<sup>-2</sup></td><td>90</td><td>14 AVRORIN</td><td>14 BAIK</td><td>H, solar $\nu$ (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 8.4 &times; 10<sup>-4</sup></td><td>90</td><td>14 AVRORIN</td><td>14 BAIK</td><td>H, solar $\nu$ (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 4.48 &times; 10<sup>-4</sup></td><td>90</td><td>15 AARTSEN</td><td>13 ICCB</td><td>H, solar $\nu$ (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 1.00 &times; 10<sup>-2</sup></td><td>90</td><td>15 AARTSEN</td><td>13 ICCB</td><td>H, solar $\nu$ (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 8.9 &times; 10<sup>-4</sup></td><td>90</td><td>16 ADRIAN-MAR.13</td><td>ANTR</td><td>H, solar $\nu$ (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 2.0 &times; 10<sup>-2</sup></td><td>90</td><td>16 ADRIAN-MAR.13</td><td>ANTR</td><td>H, solar $\nu$ (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 2.3 &times; 10<sup>-4</sup></td><td>90</td><td>16 ADRIAN-MAR.13</td><td>ANTR</td><td>H, solar $\nu$ (\tau<sup>+</sup>\tau<sup>-</sup>)</td></tr><tr><td>&lt; 7.57 &times; 10<sup>-2</sup></td><td>90</td><td>17 APRILE</td><td>13 X100</td><td>Xe</td></tr><tr><td>&lt; 5.4 &times; 10<sup>-3</sup></td><td>90</td><td>18 BOLIEV</td><td>13 BAKS</td><td>H, solar $\nu$ (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 4.2 &times; 10<sup>-2</sup></td><td>90</td><td>18 BOLIEV</td><td>13 BAKS</td><td>H, solar $\nu$ (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 1.5 &times; 10<sup>-3</sup></td><td>90</td><td>18 BOLIEV</td><td>13 BAKS</td><td>H, solar $\nu$ (\tau<sup>+</sup>\tau<sup>-</sup>)</td></tr><tr><td>&lt; 2.50 &times; 10<sup>-4</sup></td><td>90</td><td>19 ABBASI</td><td>12 ICCB</td><td>H, solar $\nu$ (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 7.86 &times; 10<sup>-3</sup></td><td>90</td><td>19 ABBASI</td><td>12 ICCB</td><td>H, solar $\nu$ (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 8 &times; 10<sup>-2</sup></td><td>90</td><td>BEHNKE</td><td>12 COUP</td><td>CF<sub>3</sub>l</td></tr><tr><td>&lt; 8</td><td>90</td><td>DAW</td><td>12 DRFT</td><td>F (CF<sub>4</sub>)</td></tr><tr><td>&lt; 6 &times; 10<sup>-2</sup></td><td>90</td><td>FELIZARDO</td><td>12 SMPL</td><td>C<sub>2</sub>ClF<sub>5</sub></td></tr><tr><td>&lt; 8 &times; 10<sup>-2</sup></td><td>90</td><td>KIM</td><td>12 KIMS</td><td>Csl</td></tr><tr><td>&lt; 8 &times; 10<sup>3</sup></td><td>90</td><td>20 AHLEN</td><td>11 DMTP</td><td>F (CF<sub>4</sub>)</td></tr><tr><td>&lt; 0.4</td><td>90</td><td>BEHNKE</td><td>11 COUP</td><td>CF<sub>3</sub>l</td></tr><tr><td>&lt; 2 &times; 10<sup>-3</sup></td><td>90</td><td>21 TANAKA</td><td>11 SKAM</td><td>H, solar $\nu$ (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 2 &times; 10<sup>-2</sup></td><td>90</td><td>21 TANAKA</td><td>11 SKAM</td><td>H, solar $\nu$ (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 1 &times; 10<sup>-3</sup></td><td>90</td><td>22 ABBASI</td><td>10 ICCB</td><td>KK dark matter</td></tr><tr><td>&lt; 2 &times; 10<sup>4</sup></td><td>90</td><td>20 MIUCHI</td><td>10 NAGE</td><td>CF<sub>4</sub></td></tr><tr><td>&lt; 8.7 &times; 10<sup>-4</sup></td><td>90</td><td>ABBASI</td><td>09b ICCB</td><td>H, solar $\nu$ (W<sup>+</sup>W<sup>-</sup>)</td></tr><tr><td>&lt; 2.2 &times; 10<sup>-2</sup></td><td>90</td><td>ABBASI</td><td>09b ICCB</td><td>H, solar $\nu$ (b<sup>&#x212D;</sup>)</td></tr><tr><td>&lt; 3</td><td>90</td><td>ARCHAMBAU.,09</td><td>09A PICA</td><td>F</td></tr><tr><td>&lt; 6</td><td>90</td><td>LEBEDENKO</td><td>09A ZEP3</td><td>Xe</td></tr><tr><td>&lt; 9</td><td>90</td><td>ANGLE</td><td>08A XE10</td><td>Xe</td></tr><tr><td>&lt;100</td><td>90</td><td>ALNER</td><td>07 ZEP2</td><td>Xe</td></tr><tr><td>&lt; 0.8</td><td>90</td><td>LEE</td><td>07A KIMS</td><td>Csl</td></tr><tr><td>&lt; 4 &times; 10<sup>4</sup></td><td>90</td><td>20 MIUCHI</td><td>07 NAGE</td><td>F (CF<sub>4</sub>)</td></tr><tr><td>&lt; 30</td><td>90</td><td>23 AKERIB</td><td>06 CDMS</td><td>73<sub>Ge</sub>, 29<sub>Si</sub></td></tr><tr><td>&lt; 1.5</td><td>90</td><td>ALNER</td><td>05 NAIA</td><td>NaI</td></tr><tr><td>&lt; 15</td><td>90</td><td>BARNABE-HE.,05</td><td>05A PICA</td><td>F (C<sub>4</sub>F<sub>10</sub>)</td></tr><tr><td>&lt;600</td><td>90</td><td>BENOIT</td><td>05 EDEL</td><td>73<sub>Ge</sub></td></tr><tr><td>&lt; 10</td><td>90</td><td>GIRARD</td><td>05 SMPL</td><td>F (C<sub>2</sub>ClF<sub>5</sub>)</td></tr><tr><td>&lt;260</td><td>90</td><td>MIUCHI</td><td>03 BOLO</td><td>LiF</td></tr><tr><td>&lt;150</td><td>90</td><td>TAKEDA</td><td>03 BOLO</td><td>NaF</td></tr></tbody></table>

1 AALBERS 23 yield first SD LZ limits on WIMP-p scatter using Xe. $\sigma^{SD}(\chi p) < 2 \times 10^{-3}$ pb for m(χ) = 1 TeV.

2 ADHIKARI 23c search for SD WIMP scatter on I. No signal observed. Require $\sigma^{SD}(\chi p) < 0.2$ pb for m(χ) = 1 TeV.

3 HUANG 22 search for SD DM scatter on Xe; no signal observed; limits placed in $\sigma(\chi n)$ vs. m(DM) plane; quoted limit is for m(DM) = 1 TeV.

4 IKEDA 21 use direction sensitive TPC NEWAGE to search for SD WIMPs. No signal observed. Limits set in $\sigma^{SD}(\chi p)$ vs. m plane; $\sigma^{SD}(\chi p) < 200$ pb for m(DM) = 1000 GeV.

5 AARTSEN 20c place combined IceCube and Pico-60 velocity-independent limits on spin-dependent WIMP-p scatter $\sigma^{SD}(\chi p) < 3 \times 10^{-3}$ pb for m(WIMP) = 1 TeV assuming dominant annihilation to W.W.

6 AMOLE 19 search for SD WIMP scatter on $C_3F_8$ in PICO-60 bubble chamber; no signal: set limit for spin dependent coupling $\sigma^{SD}(\chi p) < 3 \times 10^{-4}$ pb for m(χ) = 1000 GeV.

7 APRILE 19a search for SD WIMP scatter on 1 t yr Xe; no signal, limits placed in $\sigma^{SD}(\chi p)$ vs. m(χ) plane for m ~ 6–1000 GeV.

8 XIA 19A search for WIMP scatter on Xe in Panda-II; limits placed in $\sigma^{SD}(\chi p)$ vs. m(χ) plane for m(χ) ~ 5–1 × 10⁵ GeV.
⁹ ALBERT 18c 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 σSD(χp).

¹⁰ AARTSEN 17A search for neutrinos from solar WIMP annihilation into τ⁺τ⁻ in 532 days of live time.

¹¹ AKERIB 17A search for SD WIMP scatter on Xe using 129.5 kg yr exposure; limits placed in σSD(χp) vs. m(χ) plane for m(χ) ~ 6-1 × 10⁵ GeV.

¹² FU 17 search for SD WIMP scatter on Xe; limits set in σSD(χp) vs. m(χ) plane for m(χ) ~ 4-1 × 10³ GeV.

¹³ ADRIAN-MARTINEZ 16b search for secluded DM via WIMP annihilation in solar core into light mediator which later decays to μ or νs; limits presented in Figures 3 and 4.

¹⁴ AVRINOR 14 search for neutrinos from the Sun arising from the pair annihilation of X⁰ trapped by the Sun in data taken between 1998 and 2003. See their Table 1 for limits assuming annihilation into neutrino pairs.

¹⁵ AARTSEN 13 search for neutrinos from the Sun arising from the pair annihilation of X⁰ trapped by the Sun in data taken between June 2010 and May 2011.

¹⁶ ADRIAN-MARTINEZ 13 search for neutrinos from the Sun arising from the pair annihilation of X⁰ trapped by the Sun in data taken between Jan. 2007 and Dec. 2008.

¹⁷ The value has been provided by the authors. APRILE 13 note that the proton limits on Xe are highly sensitive to the theoretical model used. See also APRILE 14a.

¹⁸ BOLIEV 13 search for neutrinos from the Sun arising from the pair annihilation of X⁰ trapped by the Sun in data taken from 1978 to 2009. See also SUVOROVA 13 for an older analysis of the same data.

¹⁹ ABBASI 12 search for neutrinos from the Sun arising from the pair annihilation of X⁰ trapped by the Sun. The amount of X⁰ depends on the X⁰-proton cross section.

²⁰ Use a direction-sensitive detector.

²¹ TANAKA 11 search for neutrinos from the Sun arising from the pair annihilation of X⁰ trapped by the Sun. The amount of X⁰ depends on the X⁰-proton cross section.

²² ABBASI 10 search for νµ from annihilations of Kaluza-Klein photon dark matter in the Sun.

²³ See also AKERIB 05.

Spin-Dependent Cross Section Limits
for Dark Matter Particle (X⁰) on Neutron

For mₓ₀ in GeV range

We provide here limits for mₓ₀ < 5 GeV

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 1 × 10<sup>2</sup></td><td>90</td><td>1 AALBERS</td><td>23A</td><td>LZ SD scatter on Xe</td></tr><tr><td>&lt; 1 × 10<sup>6</sup></td><td>90</td><td>2 ANGLOHER</td><td>22</td><td>CRES SD limit using Li</td></tr><tr><td>&lt;570</td><td>90</td><td>3 ANGLOHER</td><td>22a</td><td>CRES SD limit using Li and Al</td></tr><tr><td>&lt; 1 × 10<sup>8</sup></td><td>90</td><td>4 ABDELHAMEED</td><td>20A</td><td>CRES LiAlO<sub>2</sub></td></tr><tr><td>&lt; 1 × 10<sup>10</sup></td><td>95</td><td>5 ABDELHAMEED</td><td>19</td><td>CRES SD low mass DM on Li</td></tr><tr><td>&lt; 2.3 × 10<sup>2</sup></td><td>90</td><td>6 APRILE</td><td>19c</td><td>XE1T light DM on Xe via Migdal/bremg effect</td></tr><tr><td>&lt; 1 × 10<sup>-2</sup></td><td>90</td><td>7 APRILE</td><td>19d</td><td>XE1T light DM on Xe via ionization</td></tr><tr><td>&lt; 4 × 10<sup>4</sup></td><td>90</td><td>8 ARMENGAUD</td><td>19</td><td>EDEL GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 8 × 10<sup>-2</sup></td><td>90</td><td>9 XIA</td><td>19a</td><td>PNDX SD WIMP on Xe</td></tr><tr><td>&lt; 3</td><td>90</td><td>10 AGNESE</td><td>18</td><td>SCDM GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 3</td><td>90</td><td>11 JIANG</td><td>18</td><td>CDEX GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 10</td><td>90</td><td>12 YANG</td><td>18</td><td>CDEX WIMPs on Ge</td></tr><tr><td>&lt; 1 × 10<sup>-1</sup></td><td>90</td><td>13 AKERIB</td><td>17A</td><td>LUX Xe</td></tr><tr><td>&lt; 0.1</td><td>90</td><td>14 FU</td><td>17</td><td>PNDX SD WIMP on Xe</td></tr><tr><td>&lt; 20</td><td>90</td><td>15 ZHAO</td><td>16</td><td>CDEX GeV-scale WIMPs on Ge</td></tr><tr><td>&lt;150</td><td>90</td><td>16 AHMED</td><td>11b</td><td>CDM2 GeV-scale WIMPs on Ge</td></tr></tbody></table>

¹ AALBERS 23A search for GeV-scale WIMP scatter on Xe. No signal observed. Limits placed in σSD(χn) vs. m(χ) plane. Quoted limit is for m(χ) = 1 GeV via Migdal scattering.

² ANGLOHER 22 search for SD WIMP scatter on Li target; no signal detected; limits placed on WIMP-neutron SD scatter versus m(WIMP) = 1 GeV.

³ ANGLOHER 22a search for spin-dependent DM scatter on Li and Al for m(DM) ~ 0.2-6 GeV; no signal observed; limits set in σ(χn) vs. m(DM) plane; quoted limit is for m(DM) = 1 GeV.

⁴ ABDELHAMEED 20A use LiAlO₂ target in CRESST to search for SD WIMP scatter; no signal; quoted limit is for m(DM) = 1 GeV.

⁵ ABDELHAMEED 19 search for GeV-scale WIMP SD scatter on 7Li crystal; set limit σSD(χn) for m(χ) ~ 0.8-20 GeV; quoted limit for m(χ) = 1 GeV.

⁶ APRILE 19C search for light DM on Xe via Migdal/bremsstrahlung effect; no signal, require σSD(χn) < 230 pb for m(χ) = 1 GeV.

⁷ APRILE 19D search for light DM scatter on Xe via ionization; no signal, limits placed in σ vs. m(DM) ~ 3-6 GeV; quoted limit is for m(χ) = 1 GeV.

⁸ ARMENGAUD 19 search for GeV scale WIMP scatter on Ge; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 0.5-10 GeV; quoted limit is for m(χ) = 5 GeV.

⁹ XIA 19A search for WIMP scatter on Xe in PandaX-II; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV; quoted limit is for m(χ) = 5 GeV.

¹⁰ AGNESE 18 search for GeV scale WIMPs scatter at CDMSlite; limits placed in σSD(χn) vs. m(χ) plane for m ~ 1.5-20 GeV; quoted limit is for m(χ) = 5 GeV.

¹¹ JIANG 18 search for GeV scale WIMP scatter on Ge; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 3-10 GeV; quoted limit is for m(χ) = 5 GeV.

¹² YANG 18 search for WIMP scatter on Ge; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 2-10 GeV; quoted limit is for m(χ) = 5 GeV.

¹³ AKERIB 17A search for SD WIMP scatter on Xe with 129.5 kg yr exposure; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV; quoted limit is for m(χ) = 5 GeV.

¹⁴ FU 17 search for SD WIMP scatter on Xe; limits set in σSD(χn) vs. m(χ) plane for m(χ) ~ 4-1 × 10³ GeV; quoted limit is for m(χ) = 5 GeV.

¹⁵ ZHAO 16 search for GeV-scale WIMP scatter on Ge; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 4-30 GeV; quoted limit is for m(χ) = 5 GeV.

¹⁶ AHMED 11b search for GeV scale WIMP scatter on Ge in CDMS II; limits placed in σSD(χn) vs. m(χ) plane for m ~ 4-12 GeV. Limit given for m(χ) = 5 GeV.

For mₓ₀ = 20 GeV

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 2 × 10<sup>-6</sup></td><td>90</td><td>1 AALBERS</td><td>23</td><td>LZ SD scatter on Xe</td></tr><tr><td>&lt; 5 × 10<sup>6</sup></td><td>90</td><td>2 ANGLOHER</td><td>22</td><td>CRES SD limit using Li</td></tr><tr><td>&lt; 7 × 10<sup>-6</sup></td><td>90</td><td>3 HUANG</td><td>22</td><td>PNDX SD DM limits</td></tr><tr><td>&lt; 5 × 10<sup>7</sup></td><td>90</td><td>4 ABDELHAMEED</td><td>20A</td><td>CRES LiAlO<sub>2</sub></td></tr><tr><td>&lt; 1 × 10<sup>-1</sup></td><td>90</td><td>5 FELIZARDO</td><td>20</td><td>SMPL WIMPs via SIMPLE</td></tr><tr><td>&lt; 8 × 10<sup>-6</sup></td><td>90</td><td>6 APRILE</td><td>19A</td><td>XE1T Xe, SD</td></tr><tr><td>&lt; 3 × 10<sup>-5</sup></td><td>90</td><td>7 XIA</td><td>19A</td><td>PNDX SD WIMP on Xe</td></tr><tr><td>&lt; 1.5</td><td>95</td><td>8 AGNESE</td><td>18</td><td>SCDM Xe</td></tr><tr><td>&lt; 2.5 × 10<sup>-5</sup></td><td>90</td><td>9 AKERIB</td><td>17A</td><td>LUX Xe</td></tr><tr><td>&lt; 7 × 10<sup>-5</sup></td><td>90</td><td>10 FU</td><td>17</td><td>PNDX SD WIMP on Xe</td></tr><tr><td>&lt; 2</td><td>90</td><td>11 ZHAO</td><td>16</td><td>CDEX GeV-scale WIMPs on Ge</td></tr><tr><td>&lt; 0.09</td><td>90</td><td>12 UCHIDA</td><td>14</td><td>XMAS 129Xe, inelastic</td></tr><tr><td>&lt; 8</td><td>90</td><td>13 APRILE</td><td>13</td><td>X100 Xe</td></tr><tr><td>&lt; 0.02</td><td>90</td><td>AKIMOV</td><td>12</td><td>ZEP3 Xe</td></tr><tr><td>&lt; 0.06</td><td>90</td><td>AHMED</td><td>09</td><td>CDM2 Ge</td></tr><tr><td>&lt; 0.04</td><td>90</td><td>LEBEDENKO</td><td>09A</td><td>ZEP3 Xe</td></tr><tr><td>&lt; 50</td><td>90</td><td>14 LIN</td><td>09</td><td>TEXO Xe</td></tr><tr><td>&lt; 6 × 10<sup>-3</sup></td><td>90</td><td>ANGLE</td><td>08A</td><td>XE10 Xe</td></tr><tr><td>&lt; 0.5</td><td>90</td><td>ALNER</td><td>07</td><td>ZEP2 Xe</td></tr><tr><td>&lt; 25</td><td>90</td><td>LEE</td><td>07A</td><td>KIMS Csl</td></tr><tr><td>&lt; 0.3</td><td>90</td><td>15 AKERIB</td><td>06</td><td>CDMS 73Ge, 29Si</td></tr><tr><td>&lt; 30</td><td>90</td><td>SHIMIZU</td><td>06A</td><td>CNTR F (CaF<sub>2</sub>)</td></tr><tr><td>&lt; 60</td><td>90</td><td>ALNER</td><td>05</td><td>NAIA NaI</td></tr><tr><td>&lt; 20</td><td>90</td><td>BARNABAE-HE</td><td>05</td><td>PICA F (C<sub>4</sub>F<sub>10</sub>)</td></tr><tr><td>&lt; 10</td><td>90</td><td>BENOIT</td><td>05</td><td>EDEL 73Ge</td></tr><tr><td>&lt; 4</td><td>90</td><td>KLAPDOR-K</td><td>05</td><td>HDMS 73Ge (enriched)</td></tr><tr><td>&lt;600</td><td>90</td><td>TAKEDA</td><td>03</td><td>BOLO NaF</td></tr></tbody></table>

¹ AALBERS 23 yield first LZ limits on SD WIMP-n scatter using Xe. σSD(χn) < 2 × 10⁻⁶ pb for m(χ) = 20 GeV.

² ANGLOHER 22 search for SD WIMP-neutron scatter from Li target; no signal detected; limits placed in σ vs. m(WIMP) plane.

³ HUANG 22 search for SD DM scatter on Xe; no signal observed; limits placed in σ(χn) vs. m(DM) plane; quoted limit is for m(DM) = 20 GeV.

⁴ ABDELHAMEED 20A use LiAlO₂ target in CRESST to search for SD WIMP scatter on n; limits placed for m(WIMP): 0.3-30 GeV in Fig. 8. Quoted limit is for M(WIMP) = 30 GeV.

⁵ FELIZARDO 20 presents 2014 SIMPLE bounds on WIMP DM using C₂ClF₅ target.

⁶ APRILE 19A search for SD WIMP scatter on 1 t yr Xe; no signal: limits placed in σSD(χn) vs. m(χ) plane for m ~ 6-1000 GeV.

⁷ XIA 19A search for SD WIMP scatter on Xe in PandaX-II; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV.

⁸ AGNESE 18 give limits for σSD(χn) for m(WIMP) between 1.5 and 20 GeV using CDMSlite mode data.

⁹ AKERIB 17A search for SD WIMP scatter on Xe with 129.5 kg yr exposure; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV.

¹⁰ FU 17 search for SD WIMP scatter on Xe; limits set in σSD(χn) vs. m(χ) plane for m(χ) ~ 4-1 × 10³ GeV.

¹¹ ZHAO 16 search for GeV-scale WIMP scatter on Ge; limits placed in σSD(χn) vs. m(χ) plane for m(χ) ~ 4-30 GeV.

¹² Derived limit from search for inelastic scattering X⁰ + 129Xe → X⁰ + 129Xe*(39.58 keV).

¹³ The value has been provided by the authors. See also APRILE 14a.

¹⁴ See their Fig. 6(b) for cross section limits for mₓ₀ extending down to 2 GeV.

¹⁵ See also AKERIB 05.

For mₓ₀ = 100 GeV

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 5 × 10<sup>-6</sup></td><td>90</td><td>1 AALBERS</td><td>23</td><td>LZ SD scatter on Xe</td></tr><tr><td>&lt; 1 × 10<sup>-5</sup></td><td>90</td><td>2 HUANG</td><td>22</td><td>PNDX SD DM limits</td></tr><tr><td>&lt; 1.5 × 10<sup>-1</sup></td><td>90</td><td>3 FELIZARDO</td><td>20</td><td>SMPL WIMPs via SIMPLE</td></tr><tr><td>&lt; 1.5 × 10<sup>-5</sup></td><td>90</td><td>4 APRILE</td><td>19A</td><td>XE1T Xe, SD</td></tr><tr><td>&lt; 4 × 10<sup>-3</sup></td><td>90</td><td>5 SUZUKI</td><td>19</td><td>XMAS 129Xe, inelastic</td></tr><tr><td>&lt; 2 × 10<sup>-5</sup></td><td>90</td><td>6 XIA</td><td>19A</td><td>PNDX SD WIMP on Xe</td></tr><tr><td>&lt; 2.5 × 10<sup>-5</sup></td><td>90</td><td>7 AKERIB</td><td>17A</td><td>LUX Xe</td></tr><tr><td>&lt; 7 × 10<sup>-5</sup></td><td>90</td><td>8 FU</td><td>17</td><td>PNDX SD WIMP on Xe</td></tr><tr><td>&lt; 0.1</td><td>90</td><td>11 FELIZARDO</td><td>14</td><td>SMPL C₂ClF₅</td></tr><tr><td>&lt; 0.05</td><td>90</td><td>9 UCHIDA</td><td>14</td><td>XMAS 129Xe, inelastic</td></tr><tr><td>&lt; 4.68 × 10<sup>-4</sup></td><td>90</td><td>10 APRILE</td><td>13</td><td>X100 Xe</td></tr><tr><td>&lt; 0.01</td><td>90</td><td>AKIMOV</td><td>12</td><td>ZEP3 Xe</td></tr><tr><td>&lt; 0.01</td><td>90</td><td>11 FELIZARDO</td><td>10</td><td>SMPL C₂ClF₃</td></tr><tr><td>&lt; 0.02</td><td>90</td><td>AHMED</td><td>09</td><td>CDM2 Ge</td></tr><tr><td>&lt; 0.01</td><td>90</td><td>LEBEDENKO</td><td>09A</td><td>ZEP3 Xe</td></tr><tr><td>&lt;100</td><td>90</td><td>LIN</td><td>09</td><td>TEXO Ge</td></tr><tr><td>&lt; 0.01</td><td>90</td><td>ANGLE</td><td>08A</td><td>XE10 Xe</td></tr><tr><td>&lt; 0.05</td><td>90</td><td>12 BEDNYAKOV</td><td>08</td><td>RVUE Ge</td></tr><tr><td>&lt; 0.08</td><td>90</td><td>ALNER</td><td>07</td><td>ZEP2 Xe</td></tr><tr><td>&lt; 6</td><td>90</td><td>LEE</td><td>07A</td><td>KIMS Csl</td></tr><tr><td>&lt; 0.07</td><td>90</td><td>13 AKERIB</td><td>06</td><td>CDMS 73Ge, 29Si</td></tr><tr><td>&lt; 30</td><td>90</td><td>SHIMIZU</td><td>06A</td><td>CNTR F (CaF<sub>2</sub>)</td></tr><tr><td>&lt; 10</td><td>90</td><td>ALNER</td><td>05</td><td>NAIA NaI</td></tr><tr><td>&lt; 30</td><td>90</td><td>BARNABAE-HE</td><td>05</td><td>PICA F (C<sub>4</sub>F<sub>10</sub>)</td></tr><tr><td>&lt; 0.7</td><td>90</td><td>BENOIT</td><td>05</td><td>EDEL 73Ge</td></tr></tbody></table>
# Searches Particle Listings
## WIMP and Dark Matter Searches

<table><tr><td>&lt; 0.2</td><td></td></tr><tr><td>&lt; 1.5</td><td>90</td></tr><tr><td>&lt;800</td><td>90</td></tr></table>

<table><tr><td>14 GIULIANI</td><td>05A</td><td>RVUE</td></tr><tr><td>15 GIULIANI</td><td>04</td><td>RVUE</td></tr><tr><td>16 GIULIANI</td><td>04A</td><td>RVUE</td></tr><tr><td>17 MIUCHI</td><td>03</td><td>BOLO LiF</td></tr><tr><td></td><td></td><td>TAKEDA</td></tr><tr><td></td><td></td><td>BOLO NaF</td></tr></table>

<table><tr><td>&lt;1000</td><td>90</td></tr><tr><td>&lt; 2 &times; 10<sup>-9</sup></td><td>95</td></tr><tr><td>&lt; 100</td><td></td></tr></table>

<table><tr><td>4 AGOSTINI</td><td>22A</td><td>GERD</td><td>search for superWIMPs</td></tr><tr><td>5 APRILE</td><td>22</td><td>XEIT</td><td>WIMP-e scatter</td></tr><tr><td>6 BATTAGLIERI</td><td>22</td><td></td><td>BDX-MINI search for light DM from beam dump</td></tr><tr><td>7 BOSE</td><td>22</td><td></td><td>DM-e limits from solar γs</td></tr><tr><td>8 GHOSH</td><td>22</td><td></td><td>boosted DM-e/DM-ν scatter</td></tr><tr><td>9 HOCHBERG</td><td>22</td><td>NSNP</td><td>superconducting nanowire search for light DM</td></tr><tr><td>10 ZHANG</td><td>22A</td><td>CDEX</td><td>light DM search on e in Ge</td></tr><tr><td>11 CHENG</td><td>21</td><td>PNDX</td><td>MeV-scale DM on e</td></tr><tr><td>12 AKERIB</td><td>20</td><td>LUX</td><td>mirror DM with Xe</td></tr><tr><td>13 AMARAL</td><td>20</td><td>SCDM</td><td>light DM scatter on e in Si</td></tr><tr><td>14 APRILE</td><td>20</td><td>XEIT</td><td>excess keV electron recoil in Xe</td></tr><tr><td>15 ARNAUD</td><td>20</td><td>EDEL</td><td>MeV DM scatter on e in Ge</td></tr><tr><td>16 BARAK</td><td>20</td><td>SENS</td><td>MeV scale DM scatter from e in Si</td></tr><tr><td>17 ABRAMOFF</td><td>19</td><td>SENS</td><td>WIMP-e scatter on Si</td></tr><tr><td>18 AGUILAR-AR...</td><td>19A</td><td>DMIC</td><td>MeV scale DM scatter on e in Si</td></tr><tr><td>19 APRILE</td><td>19D</td><td>XEIT</td><td>light DM on Xe via ionization</td></tr><tr><td>&lt; 1 &times; 10<sup>-4</sup></td><td>90</td><td></td><td></td></tr><tr><td>&lt; 0.6</td><td>90</td><td></td><td></td></tr><tr><td>&lt; 2 &times; 10<sup>6</sup></td><td>90</td><td></td><td></td></tr><tr><td>&lt; 1 &times; 10<sup>-4</sup></td><td>90</td><td></td><td></td></tr><tr><td>&lt; 9 &times; 10<sup>-3</sup></td><td>90</td><td></td><td></td></tr><tr><td>&lt; 1 &times; 10<sup>4</sup></td><td>90</td><td></td><td></td></tr><tr><td>&lt; 5 &times; 10<sup>3</sup></td><td>90</td><td></td><td></td></tr><tr><td>23 APRILE</td><td>17</td><td>X100</td><td>Xe, annual modulation</td></tr></table>

1 AALBERS 23 yield first LZ limits on SD WIMP-n scatter using Xe. $\sigma(\chi n) < 5 \times 10^{-6}$ pb for m(χ) = 100 GeV.

2 HUANG 22 search for SD DM scatter on Xe; no signal observed; limits placed in $\sigma(\chi n)$ vs. m(DM) plane; quoted limit is for m(DM) = 100 GeV.

3 FELIZARDO 20 presents 2014 SIMPLE bounds on WIMP DM using $C_2CIF_5$ target.

4 APRILE 19A search for SD WIMP scatter on 1 t yr Xe; no signal, limits placed in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m ~ 6-1000 GeV.

5 SUZUKI 19 search in single phase liquid xenon detector for inelastic scattering $\chi^0 + 129\text{Xe} \rightarrow \chi^0 + 129\text{Xe}^* (39.58 \text{ keV})$; no signal: require $\sigma(\chi n)^{SD} < 4 \times 10^{-3}$ pb for m(χ) = 100 GeV.

6 XIA 19A search for WIMP scatter on Xe in PandaX-II; limits placed in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV.

7 AKERIB 17A search for SD WIMP scatter on Xe with 129.5 kg yr exposure; limits placed in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV.

8 FU 17 search for SD WIMP scatter on Xe; limits set in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m(χ) ~ 4-1 × 10³ GeV.

9 UCHIDA 14 derived limit from search for inelastic scattering $\chi^0 + 129\text{Xe} \rightarrow \chi^0 + 129\text{Xe}(39.58 \text{ keV})$.

10 The value has been provided by the authors. See also APRILE 14A.

11 See their Fig. 3 for limits on spin-dependent neutron couplings for $\chi^0$ mass of 50 GeV.

12 BEDNYAKOV 08 reanalyze KLPADOR-KLEINGROTHAUS 05 and BAUDIS 01 data.

13 See also AKERIB 05.

14 GIULIANI 05A analyze available data and give combined limits.

15 GIULIANI 04 reanalyze COLLAR 00 data and give limits for spin-dependent $\chi^0$-neutron coupling.

16 GIULIANI 04A give limits for spin-dependent $\chi^0$-neutron couplings from existing data.

17 MIUCHI 03 give model-independent limit for spin-dependent $\chi^0$-proton and neutron cross sections. See their Fig. 5.

### For $m_{\chi^0} = 1$ TeV

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 5 &times; 10<sup>-5</sup></td><td>90</td><td>1 AALBERS</td><td>23</td><td>LZ SD scatter on Xe</td></tr><tr><td>&lt; 6 &times; 10<sup>-5</sup></td><td>90</td><td>2 HUANG</td><td>22</td><td>PNDX SD DM limits</td></tr><tr><td>&lt; 7 &times; 10<sup>-1</sup></td><td></td><td>3 FELIZARDO</td><td>20</td><td>SMPL WIMPs via SIMPLE</td></tr><tr><td>&lt; 1.2 &times; 10<sup>-4</sup></td><td>90</td><td>4 APRILE</td><td>19A</td><td>XEIT Xe, SD</td></tr><tr><td>&lt; 2 &times; 10<sup>-4</sup></td><td>90</td><td>5 XIA</td><td>19A</td><td>PNDX Xe</td></tr><tr><td>&lt; 2.5 &times; 10<sup>-4</sup></td><td>90</td><td>6 AKERIB</td><td>17A</td><td>LUX Xe</td></tr><tr><td>&lt; 4 &times; 10<sup>-4</sup></td><td>90</td><td>7 FU</td><td>17</td><td>PNDX SD WIMP on Xe</td></tr><tr><td>&lt; 0.07</td><td>90</td><td>FELIZARDO</td><td>14</td><td>SMPL C<sub>2</sub>CIF<sub>5</sub></td></tr><tr><td>&lt; 0.2</td><td>90</td><td>8 UCHIDA</td><td>14</td><td>XMAS 129Xe, inelastic</td></tr><tr><td>&lt; 3.64 &times; 10<sup>-3</sup></td><td>90</td><td>9 APRILE</td><td>13</td><td>X100 Xe</td></tr><tr><td>&lt; 0.08</td><td>90</td><td>AKIMOV</td><td>12</td><td>ZEP3 Xe</td></tr><tr><td>&lt; 0.2</td><td>90</td><td>AHMED</td><td>09</td><td>CDM2 Ge</td></tr><tr><td>&lt; 0.1</td><td>90</td><td>LEBEDENKO</td><td>09A</td><td>ZEP3 Xe</td></tr><tr><td>&lt; 0.1</td><td>90</td><td>ANGLE</td><td>08A</td><td>XE10 Ge</td></tr><tr><td>&lt; 0.25</td><td>90</td><td>10 BEDNYAKOV</td><td>08</td><td>RVUE Ge</td></tr><tr><td>&lt; 0.6</td><td>90</td><td>ALNER</td><td>07</td><td>ZEP2 Xe</td></tr><tr><td>&lt; 30</td><td>90</td><td>LEE</td><td>07A</td><td>KIMS Csl</td></tr><tr><td>&lt; 0.5</td><td>90</td><td>11 AKERIB</td><td>06</td><td>CDMS 73Ge, 29Si</td></tr><tr><td>&lt; 40</td><td>90</td><td>ALNER</td><td>05</td><td>NAIA NaI</td></tr><tr><td>&lt;200</td><td>90</td><td>BARNABE-HE.05</td><td>05</td><td>PICA F (C<sub>4</sub>F<sub>10</sub>)</td></tr><tr><td>&lt; 4</td><td>90</td><td>BENOIT</td><td>05</td><td>EDEL 73Ge</td></tr><tr><td>&lt; 10</td><td>90</td><td>KLPADOR-K...05</td><td>HDMS</td><td>73Ge (enriched)</td></tr><tr><td>&lt; 4 &times; 10<sup>3</sup></td><td>90</td><td>TAKEDA</td><td>03</td><td>BOLO NaF</td></tr></tbody></table>

1 AALBERS 23 yield first LZ SD limits on WIMP-n scatter on Xe. $\sigma^{SD}(\chi n) < 5 \times 10^{-5}$ pb for m(χ) = 1 TeV.

2 HUANG 22 search for SD DM scatter on Xe; no signal observed; limits placed in $\sigma(\chi n)$ vs. m(DM) plane; quoted limit is for m(DM) = 1 TeV.

3 FELIZARDO 20 presents 2014 SIMPLE bounds on WIMP DM using $C_2CIF_5$ target.

4 APRILE 19A search for SD WIMP scatter on 1 t yr Xe; no signal, limits placed in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m ~ 6-1000 GeV.

5 XIA 19A search for WIMP scatter on Xe in PandaX-II; limits placed in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV.

6 AKERIB 17A search for SD WIMP scatter on Xe with 129.5 kg yr exposure; limits placed in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m(χ) ~ 5-1 × 10⁵ GeV.

7 FU 17 search for SD WIMP scatter on Xe; limits set in $\sigma^{SD}(\chi n)$ vs. m(χ) plane for m(χ) ~ 4-1 × 10³ GeV.

8 Derived limit from search for inelastic scattering $\chi^0 + 129\text{Xe}^* \rightarrow \chi^0 + 129\text{Xe}^*(39.58 \text{ keV})$.

9 The value has been provided by the authors. See also APRILE 14A.

10 BEDNYAKOV 08 reanalyze KLPADOR-KLEINGROTHAUS 05 and BAUDIS 01 data.

11 See also AKERIB 05.

1 AGNES 23A search for MeV-scale DM scatter from e using Ar. No signal observed. $\sigma(\chi e) < 3 \times 10^{-3}$ pb for m(χ) = 30 MeV.

2 ARNQUIST 23A search for LDM scatter on e using CCDs. No signal observed. Require $\sigma(\chi e) < 0.3$ pb for m(χ) = 10 MeV and $F_{DM} = 1$ (Fig. 3b).

3 LI 23F search for light DM in MeV range via scatter from e. No signal observed. Limits set. The quoted limit is for m(χ) = 0.2 GeV with $F_{DM} = 1$.

4 AGOSTINI 22 search for superWIMP particles using GERDA detector; no signal observed; limits placed in mass vs coupling plane for m(DM) 0.06-1 MeV.

5 APRILE 22 place new limits on WIMP-e scatter for dark photon and various multipole moments vs. WIMP mass for various DM models; quoted limit for m(WIMP) = 1 GeV in light mediator model.

6 BATTAGLIERI 22 search for light MeV scale DM particles produced in JLAB beam dump; no signal observed; limits set in kinetic mixing vs. m(DM) plane for m(DM) ~ 1-200 MeV.

7 BOSE 22A theoretically derive limits on WIMP-e scatter from solar gamma rays using data of Fermi-LAT; limit quoted for m(WIMP) = 5 GeV.

8 GHOSH 22 derive limits on sub-GeV boosted DM scatter from e or ν using SuperK/XENON1T data; quoted limit for m(χ) = 1 MeV.

9 HOCHBERG 22 search for sub-eV or sub-MeV scale DM scatter/absorption on e in superconducting nanowire; no signal observed; limits set in m(DM) vs. cross section plane for sub-MeV-scale DM and in m(DM) vs. kinetic mixing plane for sub-eV-scale DM.

10 ZHANG 22A search for DM scatter on e using CDEX-10; no signal observed; limits placed on $\sigma(\chi e)$ vs. m(DM) plane for m(DM) ~ 0.07-10 GeV for various simplified models.

11 CHENG 21 search for MeV-scale DM scatter from e in PANDAX-II. No signal detected. Limits set in $\sigma(\chi e)$ vs. m(DM) plane for two choices of form factors; $\sigma(\chi e) < 10$ pb for m(χ) = 10 MeV and $F_{DM} = 1$.

12 AKERIB 20 search for mirror DM with LUX 95 d × 118 kg data for mirror e scatter from Xe; no signal, limits placed in kinetic mixing parameter vs. mirror e temperature T ~ 0.1-0.9 keV plane.

13 AMARAL 20 search SuperCDMS data for low mass DM scatter from e in Si; no signal; quoted limit $\sigma_e < 8.7 \times 10^2$ pb for m(DM) = 10 MeV with form factor $F_{DM} = 1$.

14 APRILE 20 report excess at electron recoil around 2-3 keV in Xe; data compared to unforeseen tritium background, and various signal models (bosonic DM, solar axion, and neutrino magnetic moment).

15 ARNAUD 20 search for MeV DM scattering from e in Ge; no signal; quoted limit is for m(DM) = 10 MeV with form factor $F_{DM} = 1$.

16 BARAK 20 report search for MeV scale DM scatter from e in Si; limits placed in $\sigma_e$ vs. m(DM) plane; quoted limit is for m(DM) = 10 MeV and form factor $F_{DM} = 1$.

17 ABRAMOFF 19 search for MeV-scale WIMP scatter from Si skipper-CCD; limits placed on $\sigma(\chi e)$ for m(χ) ~ 0.5-100 MeV depending on DM form factors. Limit given for m(DM) = 1 MeV.

18 AGUILAR-AREVALO 19A search for MeV scale DM scatter from e in Si CCDs at SNO-LAB; no signal, limits placed in $\sigma(\chi e)$ vs. m(DM) plane for m(DM) ~ 0.6-100 MeV.

19 APRILE 19d search for light DM scatter on Xe via ionization; no signal, limits placed in $\sigma$ on nucleus vs. m(DM) plane for m(DM) ~ 0.02-10 GeV; quoted limit is for m(DM) = 0.2 GeV.

20 AGNES 18B search for MeV scale WIMP scatter from e in Ar; no signal, limits set in $\sigma_e$ vs. m(χ) plane for m ~ 20-1000 MeV and two choices of form factor F(DM); quoted limit for m(χ) = 100 MeV and F = 1.

21 AGNESE 18B search for eχ scatter in SuperCDMS; limits placed in $\sigma(\chi e)$ vs. m(χ) plane for m ~ 0.3-1 × 10⁴ MeV for two assumed form factors and also in m(dark photon) vs. kinetic mixing plane. Limit given for m(χ) = 1 GeV and F=1.

22 CRISLER 18 search for χe → χe scatter in Si CCD; place limits on MeV DM in $\sigma_e$ vs. m(χ) plane for m ~ 0.5-1000 MeV for different form factors; quoted limit is for F(DM) = 1 and m(χ) = 10 MeV.

23 APRILE 17 search for WIMP-e annual modulation signal for recoil energy in the 2.0-5.8 keV interval using 4 years data with Xe. No significant effect seen.

### Cross-Section Limits for Dark Matter Particles ($\chi^0$) on electron

#### For $m_{\chi^0}$ in GeV range

We provide here limits for $m_{\chi^0} < 5$ GeV

<table><thead><tr><th>VALUE (pb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 3 &times; 10<sup>-3</sup></td><td>90</td><td>1 AGNES</td><td>23A</td><td>DS50 LDM scatter on e</td></tr><tr><td>0.3</td><td>90</td><td>2 ARNQUIST</td><td>23A</td><td>DAMC LDM search via CCDs</td></tr><tr><td>&lt; 2 &times; 10<sup>-5</sup></td><td>90</td><td>3 LI</td><td>23F</td><td>PNDX light DM limits</td></tr></tbody></table>

### Cross-Section Limits for Dark Matter Particles ($\chi^0$) on Nuclei

#### For $m_{\chi^0}$ in GeV range

We provide here limits for $m_{\chi^0} < 5$ GeV

<table><thead><tr><th>VALUE (pb)</th><th>DOCUMENT ID</th><th>COMMENT</th></tr></thead><tbody><tr><td>&middot;&middot;&middot;</td><td></td><td></td></tr><tr><td>&middot;&middot;&middot;</td><td>1 AKIMOV</td><td>22 COHERENT search for DM mediators</td></tr></tbody></table>

<footnote n="1">1 AKIMOV 22 use COHERENT Csl(Na) detector to search for sub GeV DM particles produced by the Spallation Neutron Source; no signal observed; limits placed in mediator mass vs. coupling plane for leptophobic DM models.</footnote>