EXOTIC BARYONS

See the related review(s):

Pentaquarks

$$P_c\bar{c}(4312)^+$$

$$I(J^P) = \frac{1}{2}(?^?) \quad \text{Status: *}$$

OMITTED FROM SUMMARY TABLE

Was $P_c(4312)^+$.

$P_c\bar{c}(4312)^+$ MASS

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>4311.9 ± 0.7 <sup>+6.8</sup><sub>-0.6</sub></td><td>AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr></tbody></table>

$P_c\bar{c}(4312)^+$ WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>9.8 ± 2.7 <sup>+3.7</sup><sub>-4.5</sub></td><td>AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr></tbody></table>

$P_c\bar{c}(4312)^+$ DECAY MODES

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>i</sub>/Γ)</th></tr></thead><tbody><tr><td>Γ<sub>1</sub> J/ψp</td><td>seen</td></tr></tbody></table>

$P_c\bar{c}(4312)^+$ BRANCHING RATIOS

<table><thead><tr><th>Γ(J/ψp)/Γ<sub>total</sub></th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>seen</td><td>246k</td><td>1 AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr></tbody></table>

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

not seen 797 2 AAIJ 22H LHCB pp at 7, 8, 13 TeV

1 Amplitude analysis of $\Lambda_b^0 \to J/\psi p K^-$.

2 Amplitude analysis of $B_s^0 \to J/\psi p \bar{p}$. AAIJ 22H finds evidence at just over 3 σ for a $J/\psi p$ structure at $4337_{-4}^{+7} \pm 2$ MeV.

$P_c\bar{c}(4312)^+$ REFERENCES

<table><tr><td>AAIJ</td><td>22H PRL 128 062001</td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr><tr><td>AAIJ</td><td>19W PRL 122 222001</td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr></table>

$$P_c\bar{c}_s(4338)^0$$

$$I(J^P) = 0(\frac{1}{2}) \quad \text{Status: *}$$

AAIJ 23Q determines that spin-parity $J^P = 1/2^-$ is preferred, while spin-parity $J^P = 1/2^+$ is excluded at a 90% confidence level and spin $J = 3/2$ hypotheses are discarded.

$P_c\bar{c}_s(4338)^0$ MASS

<table><thead><tr><th>VALUE (MeV)</th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>4338.2 ± 0.7 ± 0.4</td><td>4.4k</td><td>AAIJ</td><td>23Q</td><td>LHCB $B^- \to J/\psi \Lambda \bar{p}$</td></tr></tbody></table>

$P_c\bar{c}_s(4338)^0$ WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>7.0 ± 1.2 ± 1.3</td><td>4.4k</td><td>AAIJ</td><td>23Q</td><td>LHCB $B^- \to J/\psi \Lambda \bar{p}$</td></tr></tbody></table>

$P_c\bar{c}_s(4338)^0$ DECAY MODES

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>i</sub>/Γ)</th></tr></thead><tbody><tr><td>Γ<sub>1</sub> J/ψΛ</td><td>seen</td></tr></tbody></table>

$P_c\bar{c}_s(4338)^0$ BRANCHING RATIOS

<table><thead><tr><th>Γ(J/ψΛ)/Γ<sub>total</sub></th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>seen</td><td>4.4k</td><td>AAIJ</td><td>23Q</td><td>LHCB $B^- \to J/\psi \Lambda \bar{p}$</td></tr></tbody></table>

$P_c\bar{c}_s(4338)^0$ REFERENCES

<table><tr><td>AAIJ</td><td>23Q PRL 131 031901</td><td>R. Aaij et al.</td><td>(LHCb Collab.) JP</td></tr></table>

$$P_c\bar{c}(4380)^+$$

$$I(J^P) = \frac{1}{2}(?^?) \quad \text{Status: *}$$

OMITTED FROM SUMMARY TABLE

Was $P_c(4380)^+$.

A resonance seen in $\Lambda_b^0 \to P_c^+ K^-$, then $P_c \to J/\psi p$, with a significance of 9 standard deviations. The $J/\psi p$ quark content is $u u d c \bar{c}$, a pentaquark. See also the $P_c(4450)^+$. In the best amplitude fit, the two states have opposite parity, one having $J = 3/2$, the other $J = 5/2$.

Extraction of the pentaquark signals requires some understanding of the dominant $K^- p$ background. AAIJ 15P used a model-dependent approach. AAIJ 16AG reanalyzed the data making minimal assumptions about the $K^- p$ background, and thus confirmed the strong significance of the pentaquark signals.

$P_c\bar{c}(4380)^+$ MASS

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>4380 ± 8 ± 29</td><td>AAIJ</td><td>15P</td><td>LHCB pp at 7, 8 TeV</td></tr></tbody></table>

$P_c\bar{c}(4380)^+$ WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>205 ± 18 ± 86</td><td>AAIJ</td><td>15P</td><td>LHCB pp at 7, 8 TeV</td></tr></tbody></table>

$P_c\bar{c}(4380)^+$ DECAY MODES

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>i</sub>/Γ)</th></tr></thead><tbody><tr><td>Γ<sub>1</sub> J/ψp</td><td>seen</td></tr></tbody></table>

$P_c\bar{c}(4380)^+$ BRANCHING RATIOS

<table><thead><tr><th>Γ(J/ψp)/Γ<sub>total</sub></th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>seen</td><td>19W</td><td>AAIJ</td><td>15P</td><td>LHCB pp at 7, 8 TeV</td></tr></tbody></table>

$P_c\bar{c}(4380)^+$ REFERENCES

<table><tr><td>AAIJ</td><td>16AG PRL 117 082002</td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr><tr><td>AAIJ</td><td>15P PRL 115 072001</td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr></table>

$$P_c\bar{c}(4440)^+$$

$$I(J^P) = \frac{1}{2}(?^?) \quad \text{Status: *}$$

OMITTED FROM SUMMARY TABLE

Was $P_c(4440)^+$.

$P_c\bar{c}(4440)^+$ MASS

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>4440.3 ± 1.3 <sup>+4.1</sup><sub>-4.7</sub></td><td>AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr></tbody></table>

$P_c\bar{c}(4440)^+$ WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>20.6 ± 4.9 <sup>+8.7</sup><sub>-10.1</sub></td><td>AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr></tbody></table>

$P_c\bar{c}(4440)^+$ DECAY MODES

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>i</sub>/Γ)</th></tr></thead><tbody><tr><td>Γ<sub>1</sub> J/ψp</td><td>seen</td></tr></tbody></table>

$P_c\bar{c}(4440)^+$ BRANCHING RATIOS

<table><thead><tr><th>Γ(J/ψp)/Γ<sub>total</sub></th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>seen</td><td>1 POPOV</td><td>21</td><td>D0</td><td>p p̄ at 1.96 TeV</td></tr><tr><td>seen</td><td>AAIJ</td><td>19W</td><td>LHCB</td><td>pp at 7, 8, 13 TeV</td></tr></tbody></table>

¹Search for $J/\psi$ inclusive production in association with a charged particle, assumed to be a proton. POPOV 21 observes a resonant signal consistent with a superposition of the $P_c\bar{c}(4440)^+$ and $P_c\bar{c}(4457)^+$, using masses and widths measured by AAIJ 19W, at significance of $3\sigma$.

$P_c\bar{c}(4440)^+$ REFERENCES

<table><tr><td>POPOV</td><td>21</td><td>PAN 83 1383</td><td></td><td></td></tr><tr><td>AAIJ</td><td>19W</td><td>PRL 122 222001</td><td>A.V. Popov et al.</td><td>(D0 Collab.)</td></tr><tr><td></td><td></td><td></td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr></table>
# Baryon Particle Listings

## $P_{c\bar{c}}(4457)^{+}$, $P_{c\bar{c}s}(4459)^{0}$

$$P_{c\bar{c}}(4457)^{+}$$

$$I(J^P) = \frac{1}{2}(?^?) \text{ Status: } *$$

OMITTED FROM SUMMARY TABLE

was $P_c(4450)$

A resonance seen in $\Lambda_b^0 \to P^+K^-$, then $P_c \to J/\psi p$, with a significance of 12 standard deviations. The $J/\psi p$ quark content is $uudc\bar{c}$, a pentaquark. See also the $P_{c\bar{c}}(4380)^{+}$. In the best amplitude fit, the two states have opposite parity, one having $J = 3/2$, the other $J = 5/2$.

Extraction of the pentaquark signals requires some understanding of the dominant $K^-p$ background. AAIJ 15P used a model-dependent approach. AAIJ 16AG reanalyzed the data making minimal assumptions about the $K^-p$ background, and thus confirmed the strong significance of the pentaquark signals.

### $P_{c\bar{c}}(4457)^{+}$ MASS

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>4457.3 ± 0.6 <sup>+4.1</sup><sub>-1.7</sub></td><td>AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr></tbody></table>

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

<table><tr><td>4449.8 ± 1.7 ± 2.5</td><td>1 AAIJ</td><td>15P</td><td>LHCB Repl. by AAIJ 19W</td></tr></table>

¹ Considering $P_{c\bar{c}}(4440)$ and $P_{c\bar{c}}(4457)$ as a single resonance.

### $P_{c\bar{c}}(4457)^{+}$ WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>6.4 ± 2.0 <sup>+ 5.7</sup><sub>- 1.9</sub></td><td>AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr></tbody></table>

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

<table><tr><td>39 ± 5 ± 19</td><td>1 AAIJ</td><td>15P</td><td>LHCB Repl. by AAIJ 19W</td></tr></table>

¹ Considering $P_{c\bar{c}}(4440)$ and $P_{c\bar{c}}(4457)$ as a single resonance.

### $P_{c\bar{c}}(4457)^{+}$ DECAY MODES

<table><thead><tr><th>Mode</th><th>Fraction ($\Gamma_j/\Gamma$)</th></tr></thead><tbody><tr><td>$\Gamma_1$ J/ψp</td><td>seen</td></tr></tbody></table>

### $P_{c\bar{c}}(4457)^{+}$ BRANCHING RATIOS

#### $\Gamma(J/\psi p)/\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>seen</td><td>1 POPOV</td><td>21</td><td>D0 pP at 1.96 TeV</td></tr><tr><td>seen</td><td>AAIJ</td><td>19W</td><td>LHCB pp at 7, 8, 13 TeV</td></tr><tr><td>seen</td><td>AAIJ</td><td>15P</td><td>LHCB pp at 7, 8 TeV</td></tr></tbody></table>

### $P_{c\bar{c}}(4457)^{+}$ REFERENCES

<table><tr><td>POPOV</td><td>21</td><td>PAN 83 1383</td><td>(D0 Collab.)</td></tr><tr><td>AAIJ</td><td>19W</td><td>PRL 122 222001</td><td>(LHCb Collab.)</td></tr><tr><td>AAIJ</td><td>16AG</td><td>PRL 117 082002</td><td>(LHCb Collab.)</td></tr><tr><td>AAIJ</td><td>15P</td><td>PRL 115 072001</td><td>(LHCb Collab.)</td></tr></table>

$$P_{c\bar{c}s}(4459)^{0}$$

$$I(J^P) = 0(?^?) \text{ Status: } *$$

OMITTED FROM SUMMARY TABLE

### $P_{c\bar{c}s}(4459)^{0}$ MASS

<table><thead><tr><th>VALUE (MeV)</th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>4458.8 ± 2.9 <sup>+4.7</sup><sub>-1.1</sub></td><td>1.8k</td><td>1 AAIJ</td><td>21AO LHCB</td><td>$\Xi_b^-$ → J/ψΛK<sup>-</sup></td></tr></tbody></table>

¹ AAIJ 21AO sees evidence for the $P_{c\bar{c}s}(4459)$ at $3.1\sigma$ global significance.

### $P_{c\bar{c}s}(4459)^{0}$ WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>17.3 ± 6.5 <sup>+8.0</sup><sub>-5.7</sub></td><td>1.8k</td><td>1 AAIJ</td><td>21AO LHCB</td><td>$\Xi_b^-$ → J/ψΛK<sup>-</sup></td></tr></tbody></table>

¹ AAIJ 21AO sees evidence for the $P_{c\bar{c}s}(4459)$ at $3.1\sigma$ global significance.

### $P_{c\bar{c}s}(4459)^{0}$ DECAY MODES

<table><thead><tr><th>Mode</th><th>Fraction ($\Gamma_j/\Gamma$)</th></tr></thead><tbody><tr><td>$\Gamma_1$ J/ψΛ</td><td>seen</td></tr></tbody></table>

### $P_{c\bar{c}s}(4459)^{0}$ BRANCHING RATIOS

#### $\Gamma(J/\psi\Lambda)/\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE</th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>seen</td><td>1.8k</td><td>1 AAIJ</td><td>21AO LHCB</td><td>$\Xi_b^-$ → J/ψΛK<sup>-</sup></td></tr></tbody></table>

¹ AAIJ 21AO sees evidence for the $P_{c\bar{c}s}(4459)$ at $3.1\sigma$ global significance.

### $P_{c\bar{c}s}(4459)^{0}$ REFERENCES

<table><tr><td>AAIJ</td><td>21AO SCIB 66 1278</td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr></table>

<footnote n="1">¹ Search for J/ψ inclusive production in association with a charged particle, assumed to be a proton. POPOV 21 observes a resonant signal consistent with a superposition of the $P_{c\bar{c}}(4440)^{+}$ and $P_{c\bar{c}}(4457)^{+}$, using masses and widths measured by AAIJ 19W, at significance of $3\sigma$.</footnote>
## MISCELLANEOUS SEARCHES

<table><tr><td>Magnetic Monopole Searches</td><td>2289</td></tr><tr><td>Supersymmetric Particle Searches</td><td>2292</td></tr><tr><td>Technicolor</td><td>2347</td></tr><tr><td>Quark and Lepton Compositeness</td><td>2348</td></tr><tr><td>Extra Dimensions</td><td>2352</td></tr><tr><td>WIMP and Dark Matter Searches</td><td>2359</td></tr><tr><td>Other Particle Searches</td><td>2374</td></tr></table>

## SEARCHES IN OTHER SECTIONS

<table><tr><td>Neutral Higgs Bosons, Searches for</td><td>1237</td></tr><tr><td>Charged Higgs Bosons (H<sup>±</sup> and H<sup>±±</sup>), Searches for</td><td>1248</td></tr><tr><td>New Heavy Bosons</td><td>1253</td></tr><tr><td>Axions (A<sup>0</sup>) and Other Very Light Bosons</td><td>1271</td></tr><tr><td>Heavy Charged Lepton Searches</td><td>1331</td></tr><tr><td>Double-β Decay</td><td>1343</td></tr><tr><td>Heavy Neutral Leptons, Searches for</td><td>1367</td></tr><tr><td>b' (Fourth Generation) Quark</td><td>1398</td></tr><tr><td>t' (Fourth Generation) Quark</td><td>1401</td></tr><tr><td>Free Quark Searches</td><td>1403</td></tr></table>

## Related Reviews in Volume 1

<table><tr><td>85. Extra dimensions (rev.)</td><td>1021</td></tr><tr><td>86. W'-boson searches (rev.)</td><td>1029</td></tr><tr><td>87. Z'-boson searches (rev.)</td><td>1033</td></tr><tr><td>88. Supersymmetry: theory (rev.)</td><td>1038</td></tr><tr><td>89. Supersymmetry: experiment (rev.)</td><td>1058</td></tr><tr><td>90. Axions and other similar particles (rev.)</td><td>1079</td></tr><tr><td>91. Quark and lepton compositeness, searches for (rev.)</td><td>1098</td></tr><tr><td>92. Dynamical electroweak symmetry breaking: implications of the H<sup>0</sup> (rev.)</td><td>1104</td></tr><tr><td>93. Grand unified theories (rev.)</td><td>1119</td></tr><tr><td>94. Leptoquarks (rev.)</td><td>1134</td></tr><tr><td>95. Magnetic monopoles (rev.)</td><td>1138</td></tr></table>
<figure><img src="image_756.png" /></figure>
# SEARCHES
not in other sections

## Magnetic Monopole Searches

See the related review(s):

Magnetic Monopoles

### Monopole Production Cross Section — Accelerator Searches

<table><thead><tr><th>X-SECT<br>(cm²)</th><th>MASS<br>(GeV)</th><th>CHG<br>(g)</th><th>ENERGY<br>(GeV)</th><th>BEAM</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&lt;4 E-41</td><td>200-4000</td><td>1-2</td><td>13000</td><td>pp</td><td>1 AAD</td><td>23CO ATLS</td></tr><tr><td>&lt;4 E-38</td><td>590-1000</td><td>1-4</td><td>8000</td><td>pp</td><td>2 ACHARYA</td><td>22A INDU</td></tr><tr><td>&lt;2 E-29</td><td>0-70</td><td>1-3</td><td>5020</td><td>PbPb</td><td>3 ACHARYA</td><td>22B INDU</td></tr><tr><td>&lt;3 E-38</td><td>750-1910</td><td>1-5</td><td>13000</td><td>pp</td><td>4 ACHARYA</td><td>21 INDU</td></tr><tr><td>&lt;1.3E-40</td><td>200-4000</td><td>1</td><td>13000</td><td>pp</td><td>5 AAD</td><td>20G ATLS</td></tr><tr><td>&lt;5.6E-40</td><td>500-4000</td><td>2</td><td>13000</td><td>pp</td><td>5 AAD</td><td>20G ATLS</td></tr><tr><td>&lt;200-5000</td><td>200-5000</td><td>2</td><td>13000</td><td>pp</td><td>6 ACHARYA</td><td>19B INDU</td></tr><tr><td>&lt;200-5000</td><td>200-5000</td><td>1</td><td>13000</td><td>pp</td><td>7 ACHARYA</td><td>18A INDU</td></tr><tr><td>&lt;2.5E-37</td><td>200-6000</td><td>1</td><td>13000</td><td>pp</td><td>8 ACHARYA</td><td>17 INDU</td></tr><tr><td>&lt;2E-37</td><td>200-6000</td><td>2</td><td>13000</td><td>pp</td><td>8 ACHARYA</td><td>17 INDU</td></tr><tr><td>&lt;4E-37</td><td>200-5000</td><td>3</td><td>13000</td><td>pp</td><td>8 ACHARYA</td><td>17 INDU</td></tr><tr><td>&lt;1.5E-36</td><td>400-4000</td><td>4</td><td>13000</td><td>pp</td><td>8 ACHARYA</td><td>17 INDU</td></tr><tr><td>&lt;7E-36</td><td>1000-3000</td><td>5</td><td>13000</td><td>pp</td><td>8 ACHARYA</td><td>17 INDU</td></tr><tr><td>&lt;5E-40</td><td>200-2500</td><td>0.5-2.0</td><td>8000</td><td>pp</td><td>9 AAD</td><td>16AB ATLS</td></tr><tr><td>&lt;2E-37</td><td>100-3500</td><td>1</td><td>8000</td><td>pp</td><td>10 ACHARYA</td><td>16 INDU</td></tr><tr><td>&lt;2E-37</td><td>100-3500</td><td>2</td><td>8000</td><td>pp</td><td>10 ACHARYA</td><td>16 INDU</td></tr><tr><td>&lt;6E-37</td><td>500-3000</td><td>3</td><td>8000</td><td>pp</td><td>10 ACHARYA</td><td>16 INDU</td></tr><tr><td>&lt;7E-36</td><td>1000-2000</td><td>4</td><td>8000</td><td>pp</td><td>10 ACHARYA</td><td>16 INDU</td></tr><tr><td>&lt;1.6E-38</td><td>200-1200</td><td>1</td><td>7000</td><td>pp</td><td>11 AAD</td><td>12CS ATLS</td></tr><tr><td>&lt;5E-38</td><td>45-102</td><td>1</td><td>206</td><td>e⁺ e⁻</td><td>12 ABBIENDI</td><td>08 OPAL</td></tr><tr><td>&lt;0.2E-36</td><td>200-700</td><td>1</td><td>1960</td><td>p̅p</td><td>13 ABULENCIA</td><td>06K CNTR</td></tr><tr><td>&lt;2E-36</td><td></td><td>1</td><td>300</td><td>e⁺ p</td><td>14,15 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;0.2E-36</td><td></td><td>2</td><td>300</td><td>e⁺ p</td><td>14,15 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;0.09E-36</td><td></td><td>3</td><td>300</td><td>e⁺ p</td><td>14,15 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;0.05E-36</td><td></td><td>≥ 6</td><td>300</td><td>e⁺ p</td><td>14,15 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;2E-36</td><td></td><td>1</td><td>300</td><td>e⁺ p</td><td>14,16 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;0.2E-36</td><td></td><td>2</td><td>300</td><td>e⁺ p</td><td>14,16 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;0.07E-36</td><td></td><td>3</td><td>300</td><td>e⁺ p</td><td>14,16 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;0.06E-36</td><td></td><td>≥ 6</td><td>300</td><td>e⁺ p</td><td>14,16 AKTAS</td><td>05A INDU</td></tr><tr><td>&lt;0.6E-36</td><td>&gt;265</td><td>1</td><td>1800</td><td>p̅p</td><td>17 KALBFLEISCH 04</td><td>INDU</td></tr><tr><td>&lt;0.2E-36</td><td>&gt;355</td><td>2</td><td>1800</td><td>p̅p</td><td>17 KALBFLEISCH 04</td><td>INDU</td></tr><tr><td>&lt;0.07E-36</td><td>&gt;410</td><td>3</td><td>1800</td><td>p̅p</td><td>17 KALBFLEISCH 04</td><td>INDU</td></tr><tr><td>&lt;0.2E-36</td><td>&gt;375</td><td>6</td><td>1800</td><td>p̅p</td><td>17 KALBFLEISCH 04</td><td>INDU</td></tr><tr><td>&lt;0.7E-36</td><td>&gt;295</td><td>1</td><td>1800</td><td>p̅p</td><td>18,19 KALBFLEISCH 00</td><td>INDU</td></tr><tr><td>&lt;7.8E-36</td><td>&gt;260</td><td>2</td><td>1800</td><td>p̅p</td><td>18,19 KALBFLEISCH 00</td><td>INDU</td></tr><tr><td>&lt;2.3E-36</td><td>&gt;325</td><td>3</td><td>1800</td><td>p̅p</td><td>18,20 KALBFLEISCH 00</td><td>INDU</td></tr><tr><td>&lt;0.11E-36</td><td>&gt;420</td><td>6</td><td>1800</td><td>p̅p</td><td>18,20 KALBFLEISCH 00</td><td>INDU</td></tr><tr><td>&lt;0.65E-33</td><td>&lt;3.3</td><td>≥ 2</td><td>11A</td><td>197 Au</td><td>21,22 HE</td><td>97</td></tr><tr><td>&lt;1.90E-33</td><td>&lt;8.1</td><td>≥ 2</td><td>160A</td><td>208 Pb</td><td>21,22 HE</td><td>97</td></tr><tr><td>&lt;3.3E-37</td><td>&lt;45.0</td><td>1.0</td><td>88-94</td><td>e⁺ e⁻</td><td>PINFOLD</td><td>93 PLAS</td></tr><tr><td>&lt;3.3E-37</td><td>&lt;41.6</td><td>2.0</td><td>88-94</td><td>e⁺ e⁻</td><td>PINFOLD</td><td>93 PLAS</td></tr><tr><td>&lt;7.E-35</td><td>&lt;44.9</td><td>0.2-1.0</td><td>89-93</td><td>e⁺ e⁻</td><td>KINOSHITA</td><td>92 PLAS</td></tr><tr><td>&lt;2.E-34</td><td>&lt;850</td><td>≥ 0.5</td><td>1800</td><td>p̅p</td><td>BERTANI</td><td>90 PLAS</td></tr><tr><td>&lt;1.2E-33</td><td>&lt;800</td><td>≥ 1</td><td>1800</td><td>p̅p</td><td>PRICE</td><td>90 PLAS</td></tr><tr><td>&lt;1.E-37</td><td>&lt;29</td><td>1</td><td>50-61</td><td>e⁺ e⁻</td><td>KINOSHITA</td><td>89 PLAS</td></tr><tr><td>&lt;1.E-37</td><td>&lt;18</td><td>2</td><td>50-61</td><td>e⁺ e⁻</td><td>KINOSHITA</td><td>89 PLAS</td></tr><tr><td>&lt;1.E-38</td><td>&lt;17</td><td>1</td><td>35</td><td>e⁺ e⁻</td><td>BRAUNSCH...</td><td>88B CNTR</td></tr><tr><td>&lt;8.E-37</td><td>&lt;24</td><td>1</td><td>50-52</td><td>e⁺ e⁻</td><td>KINOSHITA</td><td>88 PLAS</td></tr><tr><td>&lt;1.3E-35</td><td>&lt;22</td><td>2</td><td>50-52</td><td>e⁺ e⁻</td><td>KINOSHITA</td><td>88 PLAS</td></tr><tr><td>&lt;9.E-37</td><td>&lt;4</td><td>&lt;0.15</td><td>10.6</td><td>e⁺ e⁻</td><td>GENTILE</td><td>CLEO</td></tr><tr><td>&lt;3.E-32</td><td>&lt;800</td><td>≥ 1</td><td>1800</td><td>p̅p</td><td>PRICE</td><td>87 PLAS</td></tr><tr><td>&lt;3.E-38</td><td></td><td>&lt;3</td><td>29</td><td>e⁺ e⁻</td><td>FRYBERGER</td><td>84 PLAS</td></tr><tr><td>&lt;1.E-31</td><td></td><td>1,3</td><td>540</td><td>p̅p</td><td>AUBERT</td><td>83B PLAS</td></tr><tr><td>&lt;4.E-38</td><td>&lt;10</td><td>&lt;6</td><td>34</td><td>e⁺ e⁻</td><td>MUSSET</td><td>83 PLAS</td></tr><tr><td>&lt;8.E-36</td><td>&lt;20</td><td></td><td>52</td><td>pp</td><td>23 DELL</td><td>82 CNTR</td></tr><tr><td>&lt;9.E-37</td><td>&lt;30</td><td>&lt;3</td><td>29</td><td>e⁺ e⁻</td><td>KINOSHITA</td><td>82 PLAS</td></tr><tr><td>&lt;1.E-37</td><td>&lt;20</td><td>&lt;24</td><td>63</td><td>pp</td><td>CARRIGAN</td><td>78 CNTR</td></tr><tr><td>&lt;1.E-37</td><td>&lt;30</td><td>&lt;3</td><td>56</td><td>pp</td><td>HOFFMANN</td><td>78 PLAS</td></tr><tr><td></td><td></td><td></td><td>62</td><td>pp</td><td>23 DELL</td><td>78 PLAS</td></tr><tr><td></td><td></td><td></td><td>300</td><td>p</td><td>23 STEVENS</td><td>76B SPRK</td></tr><tr><td>&lt;1.E-40</td><td>&lt;5</td><td>&lt;2</td><td>70</td><td>p</td><td>24 ZRELOV</td><td>76 CNTR</td></tr><tr><td>&lt;2.E-30</td><td></td><td></td><td>300</td><td>n</td><td>23 BURKE</td><td>75 OSPK</td></tr><tr><td>&lt;1.E-38</td><td></td><td></td><td>8</td><td>ν</td><td>25 CARRIGAN</td><td>75 HLBC</td></tr><tr><td>&lt;5.E-43</td><td>&lt;12</td><td>&lt;10</td><td>400</td><td>p</td><td>EBERHARD</td><td>75B INDU</td></tr><tr><td>&lt;2.E-36</td><td>&lt;30</td><td>&lt;3</td><td>60</td><td>pp</td><td>GIACOMELLI</td><td>75 PLAS</td></tr><tr><td>&lt;5.E-42</td><td>&lt;13</td><td>&lt;24</td><td>400</td><td>p</td><td>CARRIGAN</td><td>74 CNTR</td></tr><tr><td>&lt;6.E-42</td><td>&lt;12</td><td>&lt;24</td><td>300</td><td>p</td><td>CARRIGAN</td><td>73 CNTR</td></tr><tr><td>&lt;2.E-36</td><td></td><td>1</td><td>0.001</td><td>γ</td><td>24 BARTLETT</td><td>72 CNTR</td></tr><tr><td>&lt;1.E-41</td><td>&lt;5</td><td></td><td>70</td><td>p</td><td>GUREVICH</td><td>72 EMUL</td></tr><tr><td>&lt;1.E-40</td><td>&lt;3</td><td>&lt;2</td><td>28</td><td>p</td><td>AMALDI</td><td>63 EMUL</td></tr></tbody></table>

<table><tr><td>&lt;2.E-40</td><td>&lt;3</td><td>&lt;2</td><td>30 p</td><td>PURCELL</td><td>63 CNTR</td></tr><tr><td>&lt;1.E-35</td><td>&lt;3</td><td>&lt;4</td><td>28 p</td><td>FIDECARO</td><td>61 CNTR</td></tr><tr><td>&lt;2.E-35</td><td>&lt;1</td><td>1</td><td>6 p</td><td>BRADNER</td><td>59 EMUL</td></tr></table>

1. AAD 23CO limits given for monopoles pair produced via a Drell-Yan or photon-fusion mechanism. Spins 1/2 and 0 are considered. The quoted limit is representative of the lowest values that were achieved.

2. ACHARYA 22a give limits for monopoles pair-produced via a Drell-Yan production. Spins 0, 1/2, and 1 are considered. The cross section limit is representative of the lowest values that were achieved. The experiment used a combination of nuclear track detectors to look evidence of passing monopoles and a SQUID magnetometer to look for stopped monopoles.

3. ACHARYA 22b achieved limits on monopole (point-like included) production via the Schwinger mechanism in Pb-Pb collisions at 5.02 TeV centre-of-mass energy per nucleon pair. The upper cross section limit value quoted here is representative of the lowest values achieved.

4. ACHARYA 21 search for dyons at LHC. Using a production model limits (we report the lowest) are set for dyons with magnetic charge up to 5 gD, electric charges up to 200 e and spins 0, 1/2, 1. The corresponding mass limits for magnetic monopoles are in the range 870-2040 GeV for magnetic charges in the same range.

5. AAD 20G give limits for Drell-Yan production with spin-0 and spin-1/2 monopoles. The above limit is for spin = 0 at mass = 3 TeV.

6. ACHARYA 19b limits both β-dependent and β-independent on monopoles with spins 0, 1/2, and 1 and with magnetic charges ranging from one to five times the Dirac charge in mass ranges between 200 GeV and 5000 GeV.

7. ACHARYA 18a provide limits on monopoles with spins 0, 1/2, and 1 and with magnetic charges ranging from two to five times the Dirac charge.

8. The search was sensitive to monopoles which had stopped in aluminium trapping volumes. Monopoles with spins 0 and 1/2 were considered; mass-dependent spin 1/2 monopole limits are quoted here.

9. AAD 16AB model-independent 95% CL limits estimated using a fiducial region of approximately constant acceptance. Limits are mass-dependent.

10. ACHARYA 16 limits at 95% CL estimated using a Drell-Yan-like production mechanism for scalar monopoles.

11. AAD 12CS searched for monopoles as highly ionizing objects. The cross section limits are based on an assumed Drell-Yan-like production process for spin 1/2 monopoles. The limits are mass- and scenario-dependent.

12. ABBIENDI 08 assume production of spin 1/2 monopoles with effective charge $gβ$ (n=1), via $e⁺e⁻ → γ⁺ → M̄M$, so that the cross section is proportional to $(1 + \cos^2θ)$. There is no z information for such highly saturated tracks, so a parabolic track in the jet chamber is projected onto the xy plane. Charge per hit in the chamber produces a clean separation of signal and background.

13. ABULENCIA 06k searches for high-ionizing signals in CDF central outer tracker and time-of-flight detector. For Drell-Yan $M̄M$ production, the cross section limit implies $M > 360$ GeV at 95% CL.

14. AKTAS 05A model-dependent limits as a function of monopole mass shown for arbitrary mass of 60 GeV. Based on search for stopped monopoles in the H1 Al beam pipe.

15. AKTAS 05A limits with assumed elastic spin 0 monopole pair production.

16. AKTAS 05A limits with assumed inelastic spin 1/2 monopole pair production.

17. KALBFLEISCH 04 reports searches for stopped magnetic monopoles in Be, Al, and Pb samples obtained from discarded material from the upgrading of DØ and CDF. A large-aperture warm-bore cryogenic detector was used. The approach was an extension of the methods of KALBFLEISCH 00. Cross section results moderately model dependent; Interpretation as a mass lower limit depends on possibly invalid perturbation expansion.

18. KALBFLEISCH 00 used an induction method to search for stopped monopoles in pieces of the DØ (FNAL) beryllium beam pipe and in extensions to the drift chamber aluminum support cylinder. Results are model dependent.

19. KALBFLEISCH 00 result is for aluminum.

20. KALBFLEISCH 00 result is for beryllium.

21. HE 97 used a lead target and barium phosphate glass detectors. Cross-section limits are well below those predicted via the Drell-Yan mechanism.

22. This work has also been reinterpreted in the framework of monopole production via the thermal Schwinger process (GOULD 17); this gives rise to lower mass limits.

23. Multiphoton events.

24. Cherenkov radiation polarization.

25. Re-examines CERN neutrino experiments.

### Monopole Production — Other Accelerator Searches

<table><thead><tr><th>MASS<br>(GeV)</th><th>CHG<br>(g)</th><th>SPIN</th><th>ENERGY<br>(GeV)</th><th>BEAM</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt; 610</td><td>≥ 1</td><td>0</td><td>1800 p̅p</td><td></td><td>1 ABBOTT</td><td>98K D0</td></tr><tr><td>&gt; 870</td><td>≥ 1</td><td>1/2</td><td>1800 p̅p</td><td></td><td>1 ABBOTT</td><td>98K D0</td></tr><tr><td>&gt;1580</td><td>≥ 1</td><td>1</td><td>1800 p̅p</td><td></td><td>1 ABBOTT</td><td>98K D0</td></tr><tr><td>&gt; 510</td><td></td><td></td><td>88-94 e⁺ e⁻</td><td></td><td>2 ACCIARRI</td><td>95C L3</td></tr></tbody></table>

1. ABBOTT 98K search for heavy pointlike Dirac monopoles via central production of a pair of photons with high transverse energies.

2. ACCIARRI 95C finds a limit $B(Z → γγγ)$ < 0.8 × 10⁻⁵ (which is possible via a monopole loop) at 95% CL and sets the mass limit via a cross section model.

### Monopole Flux — Cosmic Ray Searches

“Caty” in the charge column indicates a search for monopole-catalyzed nucleon decay.

<table><thead><tr><th>FLUX<br>(cm⁻²g⁻¹s⁻¹)</th><th>MASS<br>(GeV)</th><th>CHG<br>(g)</th><th>COMMENTS<br>(β = v/c)</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&lt;2E-19</td><td></td><td>1</td><td>0.86 &lt; β &lt; 0.995</td><td>1 ABBASI</td><td>22 ICCB</td></tr><tr><td>&lt;2E-14</td><td>&gt;5E8</td><td>6E-4 &lt; β &lt; 5E-3</td><td></td><td>2 ACERO</td><td>21 NOVA</td></tr><tr><td>&lt;1E-17</td><td></td><td>Caty 1E-5 &lt; β &lt; 1E-3</td><td></td><td>3 GAPONENKO</td><td>21 BAIK</td></tr><tr><td>&lt;1.5E-18</td><td></td><td>1 β &gt; 0.6</td><td></td><td>4 ALBERT</td><td>17 ANTR</td></tr><tr><td>&lt;2.5E-21</td><td></td><td>1 1E8 &lt; γ &lt; 1E13</td><td></td><td>5 AAB</td><td>16 AUGE</td></tr><tr><td>&lt;1.55E-18</td><td></td><td>β &gt; 0.51</td><td></td><td>6 AARTSEN</td><td>16B ICCB</td></tr><tr><td>&lt;1E-17</td><td></td><td>Caty 1E-3 &lt; β &lt; 1E-2</td><td></td><td>7 AARTSEN</td><td>14 ICCB</td></tr><tr><td>&lt;3E-18</td><td></td><td>1 β &gt; 0.8</td><td></td><td>8 ABBASI</td><td>13 ICCB</td></tr><tr><td>&lt;1.3E-17</td><td></td><td>1 β &gt; 0.625</td><td></td><td>9 ADRIAN-MAR..12A</td><td>ANTR</td></tr></tbody></table>
<table><tr><td>&gt;1.E+14/gram</td><td>&gt;1/3 iron aerosols</td><td>MIKHAILOV</td><td>83</td><td>SPEC</td></tr><tr><td>&lt;6.E-4/gram</td><td>air, seawater</td><td>CARRIGAN</td><td>76</td><td>CNTR</td></tr><tr><td>&lt;5.E-1/gram</td><td>&gt;0.04 11 materials</td><td>CABRERA</td><td>75</td><td>INDU</td></tr><tr><td>&lt;2.E-4/gram</td><td>&gt;0.05 moon rock</td><td>ROSS</td><td>73</td><td>INDU</td></tr><tr><td>&lt;6.E-7/gram</td><td>&lt;140 seawater</td><td>KOLM</td><td>71</td><td>CNTR</td></tr><tr><td>&lt;1.E-2/gram</td><td>&lt;120 manganese nodules</td><td>FLEISCHER</td><td>69</td><td>PLAS</td></tr><tr><td>&lt;1.E-4/gram</td><td>&gt;0 manganese</td><td>FLEISCHER</td><td>69B</td><td>PLAS</td></tr><tr><td>&lt;2.E-3/gram</td><td>&lt;1=3 magnetite, meteorite</td><td>GOTO</td><td>63</td><td>EMUL</td></tr><tr><td>&lt;2.E-2/gram</td><td>magnetite</td><td>PETUKHOV</td><td>63</td><td>CNTR</td></tr></table>

¹ Mass 1 × 10¹⁴⁻¹ × 10¹⁷ GeV.

² KOVALIK 86 examined 498 kg of schist from two sites which exhibited clear mineralogical evidence of having been buried at least 20 km deep and held below the Curie temperature.

## Monopole Density — Astrophysics

<table><thead><tr><th>DENSITY</th><th>CHG (a)</th><th>MATERIAL</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&lt;1.E-9/gram</td><td>1</td><td>sun, catalysis</td><td>1 ARAFUNE</td><td>83 COSM</td></tr><tr><td>&lt;6.E-33/nucl</td><td>1</td><td>moon wake</td><td>SCHATTEN</td><td>83 ELEC</td></tr><tr><td>&lt;2.E-28/nucl</td><td></td><td>earth heat</td><td>CARRIGAN</td><td>80 COSM</td></tr><tr><td>&lt;2.E-4/prot</td><td></td><td>42cm absorption</td><td>BRODERICK</td><td>79 COSM</td></tr><tr><td>&lt;2.E-13/m³</td><td></td><td>moon wake</td><td>SCHATTEN</td><td>70 ELEC</td></tr></tbody></table>

¹ Catalysis of nucleon decay.

## REFERENCES FOR Magnetic Monopole Searches

<table><tr><td>AAD</td><td>23CO JHEP 2311 112</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>KOBAYASHI</td><td>23A PR D108 083005</td><td>T. Kobayashi, D. Perri</td><td>(TRSTI)</td></tr><tr><td>ABBAS</td><td>22A PR P128 051101</td><td>R. Abbasi et al.</td><td>(IceCube Collab.)</td></tr><tr><td>ACHARYA</td><td>22A PR D29 694</td><td>B. Acharya et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>ACHARYA</td><td>22B NAT 602 63</td><td>B. Acharya et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>ACERO</td><td>21 PR D103 012007</td><td>M.A. Acero et al.</td><td>(NOvA Collab.)</td></tr><tr><td>ACHARYA</td><td>21 PR 126 071801</td><td>B. Acharya et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>GAPONENKO</td><td>21 PAN 84 287</td><td>O.N. Gaponenko</td><td>(ASCI)</td></tr><tr><td>AAD</td><td>20G PR D124 031802</td><td>G. Add et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>ACHARYA</td><td>19B PR 123 021802</td><td>B. Acharya et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>ACHARYA</td><td>18A PR B782 510</td><td>B. Acharya et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>ACHARYA</td><td>17 PRL 118 061801</td><td>B. Acharya et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>ALBERT</td><td>17 JHEP 1707 054</td><td>A. Abbasi et al.</td><td>(ANTARES Collab.)</td></tr><tr><td>GOLD</td><td>17 PRL 119 241601</td><td>O. Gould, A. Rajantie</td><td></td></tr><tr><td>AAB</td><td>16 PR D94 082002</td><td>A. Aad et al.</td><td>(Pierre Auger Collab.)</td></tr><tr><td>AAD</td><td>16AB PR D93 052009</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AARTSEN</td><td>16B EPJ C76 133</td><td>M.G. Aartsen et al.</td><td>(IceCube Collab.)</td></tr><tr><td>ACHARYA</td><td>16J JHEP 1608 067</td><td>M.G. Aartsen et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>AARTSEN</td><td>14 EPJ C74 2938</td><td>M.G. Aartsen et al.</td><td>(IceCube Collab.)</td></tr><tr><td>Also</td><td>13 PRL D87 022001</td><td>R. Abbasi et al.</td><td>(MoEDAL Collab.)</td></tr><tr><td>BENDTZ</td><td>13 PRL 110 121803</td><td>K. Bendtz et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>12CSD PR D92 050203</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>ADRIAN-MAR-12A</td><td>12 ASP 35 634</td><td>S. Adrian-Martinez et al.</td><td>(ANTARES Collab.)</td></tr><tr><td>UENO</td><td>12 ASP 36 131</td><td>K. Ueno et al.</td><td>(Super-Kamiokande Collab.)</td></tr><tr><td>DETRIXHE</td><td>11 PR D83 023513</td><td>M. Detrexhe et al.</td><td>(ANITA Collab.)</td></tr><tr><td>ABBASI</td><td>10A EPJ C69 361</td><td>R. Abbasi et al.</td><td>(IceCube Collab.)</td></tr><tr><td>ABBENDI</td><td>10A EPB 663 37</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>BALESTRA</td><td>08 EPJ C55 57</td><td>S. Balestra et al.</td><td>(SLIM Collab.)</td></tr><tr><td>HOGAN</td><td>08 PR D78 075531</td><td>D.P. Hogan et al.</td><td>(KANS, NEBR, DELA)</td></tr><tr><td>ABULENCIA</td><td>06K PR D96 201801</td><td>A. Abulencia et al.</td><td>(CDF Collab.)</td></tr><tr><td>AKTAS</td><td>05A EPJ C41 133</td><td>A. Aktas et al.</td><td>(H1 Collab.)</td></tr><tr><td>KALBFLEISCH</td><td>00 PR D96 052002</td><td>G.R. Kalbfleisch et al.</td><td>(OKLA)</td></tr><tr><td>AMBROSIO</td><td>02B EPJ C25 511</td><td>M. Ambrosio et al.</td><td>(MACRO Collab.)</td></tr><tr><td>AMBROSIO</td><td>02C EPJ C26 163</td><td>M. Ambrosio et al.</td><td>(MACRO Collab.)</td></tr><tr><td>AMBROSIO</td><td>02D ASP 19 27</td><td>M. Ambrosio et al.</td><td>(MACRO Collab.)</td></tr><tr><td>KALBFLEISCH</td><td>00 PR D5 85292</td><td>G.R. Kalbfleisch et al.</td><td></td></tr><tr><td>FREESE</td><td>99 PR D95 063007</td><td>K. Freese, E. Krasteva</td><td></td></tr><tr><td>ABBOTT</td><td>98K PR L81 524</td><td>B. Abbott et al.</td><td>(D0 Collab.)</td></tr><tr><td>AMBROSIO</td><td>97 PR B40 249</td><td>M. Ambrosio et al.</td><td>(MACRO Collab.)</td></tr><tr><td>HE</td><td>97 PR D93 3134</td><td>Y.D. He</td><td>(UCB)</td></tr><tr><td>ACCIARRI</td><td>95C PR B345 609</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>JEON</td><td>95 PR 75 1443</td><td>H. Jeon, M.J. Longo</td><td></td></tr><tr><td>Also</td><td>94 PR D76 159 (errat.)</td><td>H. Jeon, M.J. Longo</td><td></td></tr><tr><td>AHLEN</td><td>94 PR D21 608</td><td>S.P. Ahlen et al.</td><td>(MACRO Collab.)</td></tr><tr><td>BARISCH</td><td>94 PR D37 1306</td><td>B.C. Barish, G. Giacomelli, J.T. Hong</td><td>(CIT+)</td></tr><tr><td>BECKER-SZ...</td><td>94 PR D49 2169</td><td>A. Becker-Szendy et al.</td><td>(IMB Collab.)</td></tr><tr><td>PRICE</td><td>94 PR D37 1305</td><td>P.B. Price</td><td>(UCB)</td></tr><tr><td>ADAMS</td><td>93 PR L70 2511</td><td>F.C. Adams et al.</td><td>(MICH, FNAL)</td></tr><tr><td>PINFOLD</td><td>93 PR B316 407</td><td>J.L. Pinfold et al.</td><td>(ALBE, HARV, MONT+)</td></tr><tr><td>KINOSHITA</td><td>92 PR D46 881</td><td>K. Kinoshita et al.</td><td>(HARV, BGNA, REHO)</td></tr><tr><td>THRON</td><td>92 PR D46 4846</td><td>J.L. Thron et al.</td><td>(SOUDAN-2 Collab.)</td></tr><tr><td>GARDNER</td><td>91 PR D44 622</td><td>R.D. Gardner et al.</td><td>(STAN)</td></tr><tr><td>HUBER</td><td>91 PR D44 636</td><td>M.E. Huber et al.</td><td>(STAN)</td></tr><tr><td>ORITO</td><td>91 PR D66 1951</td><td>S. Orito et al.</td><td>(ICEPP, WASCR, NIHO, ICRR)</td></tr><tr><td>BERMON</td><td>90 PR L64 839</td><td>S. Bermon et al.</td><td></td></tr><tr><td>BERTANI</td><td>90 PR L12 613</td><td>M. Bertani et al.</td><td>(IBM, BNL)</td></tr><tr><td>BEZRUKOV</td><td>90 SJPN 52 54</td><td>L.B. Bezrukov et al.</td><td>(INRM)</td></tr><tr><td>BUCKLAND</td><td>90 PR D41 2726</td><td>K.N. Buckland et al.</td><td>(UCSD)</td></tr><tr><td>GHOSH</td><td>90 EPL 12 25</td><td>D.C. Ghosh, S. Chatterjea</td><td>(JADA)</td></tr><tr><td>HUBER</td><td>90 PR D46 835</td><td>S.TAL et al.</td><td>(STAL)</td></tr><tr><td>PRICE</td><td>90 PR L65 149</td><td>P.B. Price, J. Guiru, K. Kinoshita</td><td>(UCB, HARV)</td></tr><tr><td>KINOSHITA</td><td>89 PR B228 543</td><td>K. Kinoshita et al.</td><td>(HARV, TISA, KEK+)</td></tr><tr><td>BRAUNSCH...</td><td>88B ZPHY C38 543</td><td>R. Braunschweig et al.</td><td>(TASSO Collab.)</td></tr><tr><td>KINOSHITA</td><td>88 PR D60 1610</td><td>K. Kinoshita et al.</td><td>(HARV, TISA, KEK+)</td></tr><tr><td>BARISH</td><td>87 PR D26 2441</td><td>B. Barish, G. Liu, C. Lane</td><td>(CIT)</td></tr><tr><td>BARTELT</td><td>87 PR D39 1960</td><td>J. Bartelt et al.</td><td>(Soudan Collab.)</td></tr><tr><td>Also</td><td>87 PR D40 1701 (errat.)</td><td>J.E. Bartelt et al.</td><td>(Soudan Collab.)</td></tr><tr><td>EBISU</td><td>87 PR D36 3359</td><td>T. Ebisu, T. Watanabe</td><td>(KUBE)</td></tr><tr><td>Also</td><td>87 JP G11 883</td><td>T. Ebisu, T. Watanabe</td><td>(KUBE)</td></tr><tr><td>GENTILE</td><td>87 PR D35 1081</td><td>T. Gentile et al.</td><td>(CLEO Collab.)</td></tr><tr><td>GUY</td><td>87 NAT 325 463</td><td>J. Guy</td><td>(LOIC)</td></tr><tr><td>MASEK</td><td>87 PR D35 2758</td><td>G.E. Masek et al.</td><td>(UCSD)</td></tr><tr><td>NAKAMURA</td><td>87 PR B183 395</td><td>S. Nakamura et al.</td><td>(INUS, WASCR, NIHO)</td></tr><tr><td>PRICE</td><td>87 PRL 59 2523</td><td>P.B. Price, R. Guoxiao, K. Kinoshita</td><td>(UCB, HARV)</td></tr><tr><td>SCHOUTEN</td><td>87 JP E20 850</td><td>J.C. Schouten et al.</td><td>(LOIC)</td></tr><tr><td>SHEPKO</td><td>87 M.J. Shepko et al.</td><td>M.J. Shepko et al.</td><td>(TAMU)</td></tr><tr><td>TSUKAMOTO</td><td>87 EPL 3 39</td><td>T. Tsukamoto et al.</td><td>(ICRR)</td></tr></table>

<table><tr><td>CAPLIN</td><td>86</td><td>NAT 321 402</td><td>A.D. Caplin et al.</td><td>(LOIC)</td></tr><tr><td>Also</td><td></td><td>JP E20 850</td><td>J.C. Schouten et al.</td><td>(LOIC)</td></tr><tr><td>Also</td><td></td><td>NAT 325 463</td><td>J. Guy</td><td>(LOIC)</td></tr><tr><td>CROMAR</td><td>86</td><td>PRL 56 2561</td><td>M.W. Cromar, A.F. Clark, F.R. Fickett</td><td>(NBSB)</td></tr><tr><td>HARA</td><td>86</td><td>PRL 56 553</td><td>T. Hara et al.</td><td>(ICRR, KYOT, KEK, KOBE+)</td></tr><tr><td>INCANDELA</td><td>86</td><td>PR D34 2637</td><td>J. Incandela et al.</td><td>(CHIC, FNAL, MICH)</td></tr><tr><td>KOVALIK</td><td>86</td><td>PR A33 1183</td><td>P.B. Price, J.L. Kirschvink</td><td>(CIT)</td></tr><tr><td>PRICE</td><td>86</td><td>PRL 56 1226</td><td>M.H. Salamon</td><td>(UCB)</td></tr><tr><td>AFAUREN</td><td>85</td><td>PR D32 2586</td><td>J. Arafune, M. Fukugita, S. Yanagita</td><td>(ICRR, KYOTU+)</td></tr><tr><td>BERMON</td><td>85</td><td>PR L55 1850</td><td>S. Bermon et al.</td><td>(IBM)</td></tr><tr><td>BRACCI</td><td>85B</td><td>NP B258 726</td><td>L. Bracci, G. Fiorentini, G. Mezzorani</td><td>(PISA+)</td></tr><tr><td>Also</td><td></td><td>(PISA+)</td><td>L. Bracci, G. Fiorentini</td><td>(PISA+)</td></tr><tr><td>CAPLIN</td><td>85</td><td>NAT 317 234</td><td>A.D. Caplin et al.</td><td>(LOIC)</td></tr><tr><td>EBISU</td><td>85</td><td>JP G11 883</td><td>T. Ebisu, T. Watanabe</td><td>(KOBE)</td></tr><tr><td>KAJITA</td><td>85</td><td>JPSJ 54 4065</td><td>T. Kajita et al.</td><td>(ICRR, KEK, NIIG)</td></tr><tr><td>PARK</td><td>85B</td><td>NP B252 261</td><td>H.S. Park et al.</td><td>(IMB Collab.)</td></tr><tr><td>BATTISTONI</td><td>84</td><td>PR L33B 454</td><td>G. Battistoni et al.</td><td>(NUSEX Collab.)</td></tr><tr><td>FRYBERGER</td><td>84</td><td>PR D29 1524</td><td>D. Fryberger et al.</td><td>(SLAC, UCB)</td></tr><tr><td> Harvey</td><td>84</td><td>NP B236 255</td><td>J.A. Harvey</td><td>(PRIN)</td></tr><tr><td>INCANDELA</td><td>84</td><td>PR L53 2067</td><td>J. Incandela et al.</td><td>(CHIC, FNAL, MICH)</td></tr><tr><td>KAJINO</td><td>84</td><td>PR L52 1373</td><td>F. Kajino et al.</td><td>(ICRR)</td></tr><tr><td>KAJINO</td><td>84B</td><td>JP G10 447</td><td>F. Kajino et al.</td><td>(ICRR)</td></tr><tr><td>KAWAGDE</td><td>84</td><td>JP G10 315</td><td>K. Kawagoe et al.</td><td>(TOKY)</td></tr><tr><td>KOLB</td><td>84</td><td>APJ 286 702</td><td>E.W. Kolb, M.S. Turner</td><td>(FNAL, CHIC)</td></tr><tr><td>KRISHNA...</td><td>84</td><td>PR L42B 99</td><td>M.R. KRISHNAMOY et al.</td><td>(TATA, OSKC+)</td></tr><tr><td>LISS</td><td>84</td><td>PR D30 884</td><td>T.M. Liss, S.P. Ahlen, G. Tarle</td><td>(UCB, IND+)</td></tr><tr><td>PRICE</td><td>84</td><td>PR L52 1265</td><td>P.B. Price et al.</td><td>(ROMA, UCB, IND+)</td></tr><tr><td>PRICE</td><td>84B</td><td>PR L42 112</td><td>P.B. Price</td><td>(CERN)</td></tr><tr><td>TARLE</td><td>84</td><td>PR L52 90</td><td>G. Tarle, S.P. Ahlen, T.M. Liss</td><td>(UCB, MICH+)</td></tr><tr><td>ANDERSON</td><td>83</td><td>PR D28 2308</td><td>S.N. Anderson et al.</td><td>(WASH)</td></tr><tr><td>AFAUREN</td><td>83</td><td>PL 133B 380</td><td>J. Arafune, M. Fukugita</td><td>(ICRR, KYOTU)</td></tr><tr><td>AUBERT</td><td>83</td><td>PL 120B 465</td><td>B. Aubert et al.</td><td>(CERN, LAPP)</td></tr><tr><td>BARTWELL</td><td>83B</td><td>PL L52 955</td><td>J.E. Bartelt et al.</td><td>(MINN, ANL)</td></tr><tr><td>BARTWELL</td><td>83</td><td>PR D28 2338</td><td>S.W. Barwick, K. Kinoshita, P.B. Price</td><td>(UCB)</td></tr><tr><td>BONARELLI</td><td>82</td><td>PR L26B 137</td><td>J. Bonan et al.</td><td>(BGNA)</td></tr><tr><td>BOSETTI</td><td>83</td><td>PL 133B 265</td><td>P. Bosetti et al.</td><td>(AACH, HAWA, TOKY)</td></tr><tr><td>CABRERA</td><td>83</td><td>PL L51 1933</td><td>B. Cabrera et al.</td><td>(STAN)</td></tr><tr><td>DOKE</td><td>83</td><td>PL 129B 370</td><td>T. Doke et al.</td><td>(WASU, RIKK, TTAM, RIKEN)</td></tr><tr><td>EDRLE</td><td>83</td><td>PR L51 245</td><td>S. Freese et al.</td><td>(IMB Collab.)</td></tr><tr><td>FREESE</td><td>83B</td><td>PR L51 1625</td><td>E.M. Freese, M.S. Turner</td><td>(CHIC)</td></tr><tr><td>GROOM</td><td>83</td><td>PR L50 573</td><td>D.E. Groom et al.</td><td>(UTAH, STAN)</td></tr><tr><td>MASHIMO</td><td>83</td><td>PR L128 327</td><td>T. Mashimo et al.</td><td>(ICEPP)</td></tr><tr><td>MIKHAILEV</td><td>83</td><td>PL 130B 331</td><td>V.F. Mikhalov</td><td>(KAZA)</td></tr><tr><td>MUSSET</td><td>83</td><td>PL L128 333</td><td>P. Musset, M. Price, E. Lohrmann</td><td>(CERN, HAMB)</td></tr><tr><td>REPHAELI</td><td>83</td><td>PR L121B 115</td><td>Y. Rephael, M.S. Turner</td><td>(CHIC)</td></tr><tr><td>SCHATTEN</td><td>83</td><td>PR D27 1525</td><td>K.H. Schatten</td><td>(NASA)</td></tr><tr><td>ALEXEYEV</td><td>82</td><td>LCN 35 413</td><td>E.N. Aleksseev et al.</td><td>(INRM)</td></tr><tr><td>BONARELLI</td><td>82</td><td>PL L112B 100</td><td>R. Bonarelli et al.</td><td>(BGNA)</td></tr><tr><td>CABRERA</td><td>82</td><td>PL 48 1378</td><td>B. Cabrera et al.</td><td>(STAN)</td></tr><tr><td>DELL</td><td>82</td><td>NP B20 45</td><td>G.F. Dell et al.</td><td>(BNL, ADEL, ROMA)</td></tr><tr><td>DOIMOPOUL...</td><td>82</td><td>PL L19B 320</td><td>S. Dimopoulos, J. Preskill, F. Wilczek</td><td>(HARV+)</td></tr><tr><td>KINOSHITA</td><td>82</td><td>PL 48 77</td><td>K. Kinoshita, P.B. Price, D. Fryberger</td><td>(UCB+)</td></tr><tr><td>KOLB</td><td>82</td><td>PR L49 1373</td><td>E.W. Kolb, S.B. Colgate, J.A. Harvey</td><td>(LASL, PRIN)</td></tr><tr><td>MASHIMO</td><td>82</td><td>PSJN 51 3067</td><td>T. Mashimo, K. Kawagoe, M. Koshiba</td><td>(INUS)</td></tr><tr><td>SALPETER</td><td>82</td><td>PR L49 1114</td><td>E.L. Salpeter, S.L. Shapiro, I. Wasserman</td><td>(CORN)</td></tr><tr><td>TURNER</td><td>82</td><td>PR D26 1296</td><td>M.S. Turner, E.N. Parker, T.J. Bogdan</td><td>(CHIC)</td></tr><tr><td>BARTLETT</td><td>81</td><td>PR D24 612</td><td>D.F. Bartelt et al.</td><td>(COLO, GESC)</td></tr><tr><td>KINOSHITA</td><td>81B</td><td>PR D24 1707</td><td>K. Kinoshita, P.B. Price</td><td>(UCB)</td></tr><tr><td>ULLMAN</td><td>81</td><td>PR L47 289</td><td>J.D. Ullman</td><td>(LEHM, BNL)</td></tr><tr><td>CARRIGAN</td><td>79</td><td>PR D28 348</td><td>R.A. Carrigan</td><td>(FNAL)</td></tr><tr><td>BRODERICK</td><td>79</td><td>PR D19 1046</td><td>J.J. Broderick et al.</td><td>(VPI)</td></tr><tr><td>BARTLETT</td><td>78</td><td>PR D18 2253</td><td>D.F. Bartlett, D. Soo, M.G. White</td><td>(COLO, PRIN)</td></tr><tr><td>CARRIGAN</td><td>78</td><td>PR D17 1754</td><td>R.A. Carrigan, B.P. Strauss, G. Giacomelli</td><td>(FNAL+)</td></tr><tr><td>HOFFMANN</td><td>78</td><td>LNC 23 357</td><td>H. Hoffmann et al.</td><td>(CERN, ROMA)</td></tr><tr><td>PRICE</td><td>78</td><td>PR D18 1382</td><td>P.B. Price et al.</td><td>(UCB, HOUS)</td></tr><tr><td>HAGSTROM</td><td>77</td><td>PR L92 729</td><td>R. Hagstrom et al.</td><td>(FNAL)</td></tr><tr><td>CARRIGAN</td><td>76</td><td>PR D13 1823</td><td>R.A. Carrigan, F.A. Nezrak, B.P. Strauss</td><td>(FNAL)</td></tr><tr><td>DELL</td><td>76</td><td>LNC 15 269</td><td>G.F. Dell et al.</td><td>(CERN, BNL, ROMA, ADEL)</td></tr><tr><td>ROSS</td><td>76</td><td>PL K36-4665</td><td>R.R. Ross et al.</td><td>(LBL)</td></tr><tr><td>STEVENS</td><td>76B</td><td>PR D14 2207</td><td>D.M. Stevens et al.</td><td>(VPI, BNL)</td></tr><tr><td>ZRELVOY</td><td>76</td><td>CZJP B26 1306</td><td>V.P. Vrelko et al.</td><td>(JINR)</td></tr><tr><td>ALVAREZ</td><td>75</td><td>PL K36-4260</td><td>L.W. Alvarez</td><td>(LBL)</td></tr><tr><td>BURKE</td><td>75</td><td>PL 60B 113</td><td>D.L. Burke et al.</td><td>(MICH)</td></tr><tr><td>CABRERA</td><td>75</td><td>PL 60B 113</td><td>B. Cabrera et al.</td><td>(STAN)</td></tr><tr><td>CARRIGAN</td><td>75</td><td>NP B91 279</td><td>R.A. Carrigan, F.A. Nezrak</td><td>(FNAL)</td></tr><tr><td>Also</td><td></td><td>PR D3 56</td><td>R.A. Carrigan, F.A. Nezrak</td><td>(FNAL)</td></tr><tr><td>BERHARD</td><td>75B</td><td>PR D11 3099</td><td>P.H. Eberhard et al.</td><td>(LBL, PIM)</td></tr><tr><td>BERHARD</td><td>75B</td><td>PL B38-4289</td><td>P.H. Eberhard</td><td>(LBL)</td></tr><tr><td>FLEISCHER</td><td>75</td><td>PR D15 1412</td><td>R.L. Fleischer, R.N.F. Walker</td><td>(GESC, WUSL)</td></tr><tr><td>FRIEDLANDER</td><td>75</td><td>PR D15 1167</td><td>M.W. Friedlander</td><td>(WUSL)</td></tr><tr><td>GIACOMELLI</td><td>75</td><td>NC 28A 21</td><td>G. Giacomelli et al.</td><td>(BGNA, CERN, SACL+)</td></tr><tr><td>PRICE</td><td>75</td><td>PL D167 701</td><td>P.B. Price et al.</td><td>(UCB, HOUS)</td></tr><tr><td>CARRIGAN</td><td>74</td><td>PR D10 3867</td><td>R.A. Carrigan, F.A. Nezrak, B.P. Strauss</td><td>(FNAL)</td></tr><tr><td>CARRIGAN</td><td>73</td><td>PR D8 3717</td><td>R.A. Carrigan, F.A. Nezrak, B.P. Strauss</td><td>(FNAL)</td></tr><tr><td>ROSS</td><td>73</td><td>PR D8 3920</td><td>R.R. Ross et al.</td><td>(LBL, SLAC)</td></tr><tr><td>Also</td><td></td><td>PR D4 626</td><td>P.H. Eberhard et al.</td><td>(LBL, SLAC)</td></tr><tr><td>BARTLETT</td><td>72</td><td>PL D6 1817</td><td>L.W. Alvarez et al.</td><td>(LBL, SLAC)</td></tr><tr><td>GUREVICH</td><td>72</td><td>PL 38B 549</td><td>D.F. Bartlett, M.D. Lahana</td><td>(COLO)</td></tr><tr><td>Also</td><td></td><td>JETP 34 917</td><td>L.M. Gurevich et al.</td><td>(KIAE, NOVO, SERP)</td></tr><tr><td>Also</td><td></td><td>Translated from ZETF 61721.</td><td>L.M. Gurevich, J.I. Gurevich, M.S. Zokotorev</td><td>(KIAE+)</td></tr><tr><td>FLEISCHER</td><td>71</td><td>PR D4 24</td><td>PL 31B 394</td><td>(KIAE, NOVO, SERP)</td></tr><tr><td>KOLM</td><td>71</td><td>PR D4 1285</td><td>R.L. Fleischer et al.</td><td>(GESC)</td></tr><tr><td>PARKER</td><td>70</td><td>APJ 160 383</td><td>H.H. Kolm, F. Villa, A. Odian</td><td>(MIT, SLAC)</td></tr><tr><td>SCHATTEN</td><td>70</td><td>PR D1 2245</td><td>K.H. Schatten</td><td>(NASA)</td></tr><tr><td>FLEISCHER</td><td>70</td><td>PR D1 177 209</td><td>R.L. Fleischer et al.</td><td>(GESC, FUSU)</td></tr><tr><td>FLEISCHER</td><td>69B</td><td>PR 184 1393</td><td>R.L. Fleischer et al.</td><td>(GESC, UNCSC, GSCO)</td></tr><tr><td>FLEISCHER</td><td>69C</td><td>PR 184 1398</td><td>R.L. Fleischer, P.B. Price, R.T. Woods</td><td>(GESC)</td></tr><tr><td>Also</td><td></td><td>JAP 41 958</td><td>R.L. Fleischer et al.</td><td>(GESC)</td></tr><tr><td>CARITHERS</td><td>66</td><td>PR 149 1070</td><td>W.C.J. Carithers, R.J. Stefanski, R.K. Adair</td><td>(ROMA, UCSD, CERN)</td></tr><tr><td>AMALDI</td><td>63</td><td>PR L28 773</td><td>E. Amaldi et al.</td><td>(ROMA, UCSD, CERN)</td></tr><tr><td>GOTO</td><td>63</td><td>PR L167 387</td><td>E. Amaldi, H.H. Kolm, K.W. Ford</td><td>(TOKY, MIT, BRAN)</td></tr><tr><td>PETUKHOV</td><td>63</td><td>PR N9 87</td><td>V.A. Petukhov, M.N. Yakimenko</td><td>(LEBD)</td></tr><tr><td>PURCELL</td><td>63</td><td>PR L29 2326</td><td>E.M. Purcell et al.</td><td>(HARV, BNL)</td></tr><tr><td>FIDECARO</td><td>61</td><td>NC 22 657</td><td>M. Fidecaro, G. Finocchiaro, G. Giacomelli</td><td>(CERN)</td></tr><tr><td>BRADNER</td><td>59</td><td>PR L14 603</td><td>H. Bradner, W.M. Isbell</td><td>(LBL)</td></tr><tr><td>MALKUS</td><td>51</td><td>PR 83 899</td><td>W.V.R. Makus</td><td>(CHIC)</td></tr></table>

## OTHER RELATED PAPERS

<table><tr><td>GROOM</td><td>86</td><td>PRPL 140 323</td><td>D.E. Groom</td><td>(UTAH)</td></tr><tr><td>Review</td><td></td><td></td><td></td><td></td></tr></table>
## Supersymmetric Particle Searches

The exclusion of particle masses within a mass range ($m_1, m_2$) will be denoted with the notation “none $m_1-m_2$” in the VALUE column of the following Listings. The latest unpublished results are described in the “Supersymmetry: Experiment” review.

### See the related review(s):

Supersymmetry, Part I (Theory)

Supersymmetry, Part II (Experiment)

### CONTENTS:

- $\tilde{\chi}_1^0$ (Lightest Neutralino) mass limit

- Accelerator limits for stable $\tilde{\chi}_1^0$

- Bounds on $\tilde{\chi}_1^0$ from dark matter searches

- $\tilde{\chi}_1^0$-$p$ elastic cross section
  Spin-dependent interactions

Spin-independent interactions

- Other bounds on $\tilde{\chi}_1^0$ from astrophysics and cosmology

- Unstable $\tilde{\chi}_1^0$ (Lightest Neutralino) mass limit

- $\tilde{\chi}_2^0, \tilde{\chi}_3^0, \tilde{\chi}_4^0$ (Neutralinos) mass limits

- $\tilde{\chi}_1^\pm, \tilde{\chi}_2^\pm$ (Charginos) mass limits

- Long-lived $\tilde{\chi}^\pm$ (Chargino) mass limit

- $\tilde{\nu}$ (Sneutrino) mass limit

- Charged sleptons

- R-parity conserving $\tilde{e}$ (Selectron) mass limit

- R-parity violating $\tilde{e}$ (Selectron) mass limit

- R-parity conserving $\tilde{\mu}$ (Smuon) mass limit

- R-parity violating $\tilde{\mu}$ (Smuon) mass limit

- R-parity conserving $\tilde{\tau}$ (Stau) mass limit

- R-parity violating $\tilde{\tau}$ (Stau) mass limit

- Long-lived $\tilde{\ell}$ (Slepton) mass limit

- $\tilde{q}$ (Squark) mass limit

- R-parity conserving $\tilde{q}$ (Squark) mass limit

- R-parity violating $\tilde{q}$ (Squark) mass limit

- Long-lived $\tilde{q}$ (Squark) mass limit

- $\tilde{b}$ (Sbottom) mass limit

- R-parity conserving $\tilde{b}$ (Sbottom) mass limit

- R-parity violating $\tilde{b}$ (Sbottom) mass limit

- $\tilde{\tau}$ (Stop) mass limit

- R-parity conserving $\tilde{\tau}$ (Stop) mass limit

- R-parity violating $\tilde{\tau}$ (Stop) mass limit

- Heavy $\tilde{g}$ (Gluino) mass limit

- R-parity conserving heavy $\tilde{g}$ (Gluino) mass limit

- R-parity violating heavy $\tilde{g}$ (Gluino) mass limit

- Long-lived $\tilde{g}$ (Gluino) mass limit

- Light $\tilde{G}$ (Gravitino) mass limits from collider experiments

- Supersymmetry miscellaneous results

The results shown below, unless stated otherwise, are based on the Minimal Supersymmetric Standard Model (MSSM), as described in the Note on Supersymmetry. Unless otherwise indicated, this includes the assumption of common gaugino and scalar masses at the scale of Grand Unification (GUT), and use of the resulting relations in the spectrum and decay branching ratios. Unless otherwise indicated, it is also assumed that R-parity (R) is conserved and that:

1) The $\tilde{\chi}_1^0$ is the lowest supersymmetric particle (LSP),

2) $m_{\tilde{f}_L} = m_{\tilde{f}_R}$, where $\tilde{f}_{L,R}$ refer to the scalar partners of left- and right-handed fermions.

Limits involving different assumptions are identified in the Comments or in the Footnotes, in particular also the many simplified models, see definitions below. We summarize here the notations used in this Chapter to characterize some of the most common deviations from the MSSM (for further details, see the Note on Supersymmetry).

Theories with R-parity violation (RPV) are characterized by a superpotential of the form: $\lambda_{ijk}L_iL_je_k^c + \lambda'_{ijk}L_iQ_jd_k^c + \lambda''_{ijk}u_i^c d_j^c d_k^c$, where i, j, k are generation indices. The presence of any of these couplings is often identified in the following by the symbols $LL\bar{E}$, $LQ\bar{D}$, and $U\bar{D}\bar{D}$. Mass limits in the presence

of RPV will often refer to “direct” and “indirect” decays. Direct refers to RPV decays of the particle in consideration. Indirect refers to cases where RPV appears in the decays of the LSP. The LSP need not be the $\tilde{\chi}_1^0$.

In several models, most notably in theories with so-called Gauge Mediated Supersymmetry Breaking (GMSB), the gravitino ($\tilde{G}$) is the LSP. It is usually much lighter than any other massive particle in the spectrum, and $m_{\tilde{G}}$ is then neglected in all decay processes involving gravitinos. In these scenarios, particles other than the neutralino are sometimes considered as the next-to-lowest supersymmetric particle (NLSP), and are assumed to decay to their even-$R$ partner plus $\tilde{G}$. If the lifetime is short enough for the decay to take place within the detector, $\tilde{G}$ is assumed to be undetected and to give rise to missing energy ($E\bar{E}$) or missing transverse energy ($E\bar{T}$) signatures.

When needed, specific assumptions on the eigenstate content of $\tilde{\chi}^0$ and $\tilde{\chi}^\pm$ states are indicated, using the notation $\tilde{\gamma}$ (photino), $\tilde{H}$ (higgsino), $\tilde{W}$ (wino), and $\tilde{Z}$ (zino) to signal that the limit of pure states was used. The term gaugino is also used, to generically indicate wino-like charginos and zino-like neutralinos.

In the listings we have made use of the following abbreviations for simplified models employed by the experimental collaborations in supersymmetry searches published in the past year.

**WARNING:** Experimental lower mass limits determined within simplified models are to be treated with extreme care as they might not be directly applicable to realistic models. This is outlined in detail in the publications and we recommend consulting them before using bounds. For example, branching ratios, typically fixed to specific values in simplified models, can vary substantially in more elaborate models.

### Simplified Models Table

**Tglu1A:** gluino pair production with $\tilde{g} \to q\bar{q}\tilde{\chi}_1^0$

**Tglu1B:** gluino pair production with $\tilde{g} \to q\bar{q}'\tilde{\chi}_1^\pm$, $\tilde{\chi}_1^\pm \to W^\pm\tilde{\chi}_1^0$

**Tglu1C:** gluino pair production with a 2/3 probability of having a $\tilde{g} \to q\bar{q}'\tilde{\chi}_1^\pm$, $\tilde{\chi}_1^\pm \to W^\pm\tilde{\chi}_1^0$ decay and a 1/3 probability of having a $\tilde{g} \to q\bar{q}\tilde{\chi}_2^0$, $\tilde{\chi}_2^0 \to Z^\pm\tilde{\chi}_1^0$ decay.

**Tglu1D:** gluino pair production with one gluino decaying to $q\bar{q}'\tilde{\chi}_1^\pm$ with $\tilde{\chi}_1^\pm \to W^\pm + \tilde{G}$, and the other gluino decaying to $q\bar{q}\tilde{\chi}_1^0$ with $\tilde{\chi}_1^0 \to \gamma + \tilde{G}$.

**Tglu1E:** gluino pair production with $\tilde{g} \to q\bar{q}'\tilde{\chi}_1^\pm$, $\tilde{\chi}_1^\pm \to W^\pm\tilde{\chi}_2^0$ and $\tilde{\chi}_2^0 \to Z^\pm\tilde{\chi}_1^0$ where $m_{\tilde{\chi}_1^\pm} = (m_{\tilde{g}} + m_{\tilde{\chi}_1^0})/2$, $m_{\tilde{\chi}_2^0} = (m_{\tilde{\chi}_1^\pm} + m_{\tilde{\chi}_1^0})/2$.

**Tglu1F:** gluino pair production with $\tilde{g} \to q\bar{q}'\tilde{\chi}_1^\pm$ or $\tilde{g} \to q\bar{q}\tilde{\chi}_2^0$ with equal branching ratios, where $\tilde{\chi}_1^\pm$ decays through an intermediate scalar tau lepton or sneutrino to $\tau^+\nu\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate scalar tau lepton or sneutrino to $\tau^+\tau^-\tilde{\chi}_1^0$ or $\nu\bar{\nu}\tilde{\chi}_1^0$; the mass hierarchy is such that $m_{\tilde{\chi}_1^\pm} \sim m_{\tilde{\chi}_2^0} = (m_{\tilde{g}} + m_{\tilde{\chi}_1^0})/2$ and $m_{\tilde{\tau},\bar{\nu}} = (m_{\tilde{\chi}_1^\pm} + m_{\tilde{\chi}_1^0})/2$.

**Tglu1G:** gluino pair production with $\tilde{g} \to q\bar{q}\tilde{\chi}_2^0$, and $\tilde{\chi}_2^0$ decaying through an intermediate slepton or sneutrino to $l^+l^-\tilde{\chi}_1^0$ or $\nu\bar{\nu}\tilde{\chi}_1^0$ where $m_{\tilde{\chi}_2^0} = (m_{\tilde{g}} + m_{\tilde{\chi}_1^0})/2$ and $m_{\tilde{\ell},\bar{\nu}} = (m_{\tilde{\chi}_2^0} + m_{\tilde{\chi}_1^0})/2$.

**Tglu1H:** gluino pair production with $\tilde{g} \to q\bar{q}\tilde{\chi}_2^0$, and $\tilde{\chi}_2^0 \to \tilde{\chi}_1^0 Z^{0(*)}$.

**Tglu1I:** gluino pair production with $\tilde{g} \to q\bar{q}\tilde{\chi}_2^0$, and $\tilde{\chi}_2^0 \to \tilde{\chi}_1^0 H$.

**Tglu1J:** gluino pair production with $\tilde{g} \to q\bar{q}\tilde{\chi}_2^0$, and BR($\tilde{\chi}_2^0 \to \tilde{\chi}_1^0 Z^{0(*)}$) = BR($\tilde{\chi}_2^0 \to \tilde{\chi}_1^0 H$) = 0.5.

**Tglu1LL:** gluino pair production where $\tilde{g} \to q\bar{q}\tilde{\chi}_1^0$ happens with 1/3 probability and $\tilde{g} \to q\bar{q}\tilde{\chi}_1^\pm$ happens with 2/3 probability. The
**Tchi1n2C:** electroweak associated production of mass-degenerate charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays through an intermediate slepton or sneutrino to $l\nu\tilde{\chi}_1^0$ and where $\tilde{\chi}_1^0$ decays through an intermediate slepton or sneutrino to $l^+l^-\tilde{\chi}_1^0$ or $\nu\bar{\nu}\tilde{\chi}_1^0$ and where $m_{\tilde{\chi}_1, \tilde{\nu}} = (m_{\tilde{\chi}_1^\pm} + m_{\tilde{\chi}_1^0})/2$.

**Tchi1n2D:** electroweak associated production of mass-degenerate charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays through an intermediate scalar tau lepton or sneutrino to $\tau\nu\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate scalar tau lepton or sneutrino to $\tau^+\tau^-\tilde{\chi}_1^0$ or $\nu\bar{\nu}\tilde{\chi}_1^0$ and where $m_{\tilde{\chi}_1, \tilde{\nu}} = (m_{\tilde{\chi}_1^\pm} + m_{\tilde{\chi}_1^0})/2$.

**Tchi1n2E:** electroweak associated production of mass-degenerate charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm \to W^\pm + \tilde{\chi}_1^0$ and $\tilde{\chi}_2^0 \to H + \tilde{\chi}_1^0$.

**Tchi1n2F:** electroweak associated production of mass-degenerate wino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays through an intermediate $W^{\pm*}$ to $l\nu\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate $Z^*$ to $l^+l^-\tilde{\chi}_1^0$ or $\nu\bar{\nu}\tilde{\chi}_1^0$.

**Tchi1n2Fa:** electroweak associated production of mass-degenerate wino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays through an intermediate $W^{\pm*}$ to $l\bar{\nu}\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate $Z^*$ to $l^+l^-\tilde{\chi}_1^0$ or $\nu\bar{\nu}\tilde{\chi}_1^0$.

**Tchi1n2Fb:** electroweak associated production of mass-degenerate wino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays through an intermediate $W^{(*)}$ to $l\bar{\nu}\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate $Z^{(*)}$ to $l\bar{\nu}\tilde{\chi}_1^0$.

**Tchi1n2Fc:** electroweak associated production of mass-degenerate wino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays through an intermediate $W^{(*)}$ to $l\bar{\nu}\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate $H^{(*)}$ to $l\bar{\nu}\tilde{\chi}_1^0$.

**Tchi1n2G:** electroweak associated production of Higgsino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, and electroweak associated production of $\tilde{\chi}_2^0$ and $\tilde{\chi}_1^0$, where $m_{\tilde{\chi}_1^\pm} = (m_{\tilde{\chi}_2^0} + m_{\tilde{\chi}_1^0})/2$ and where $\tilde{\chi}_1^\pm$ decays through an intermediate $W^{\pm*}$ to $l\bar{\nu}\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate $Z^*$ to $l^+l^-\tilde{\chi}_1^0$.

**Tchi1n2Ga:** electroweak associated production of Higgsino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, and electroweak associated production of $\tilde{\chi}_2^0$ and $\tilde{\chi}_1^0$, where $m_{\tilde{\chi}_1^\pm} = (m_{\tilde{\chi}_2^0} + m_{\tilde{\chi}_1^0})/2$ and where $\tilde{\chi}_1^\pm$ decays through an intermediate $W^{\pm*}$ to $l\nu\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate $Z^*$ to $l^+l^-\tilde{\chi}_1^0$.

**Tchi1n2H:** electroweak associated production of mass-degenerate charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays through an intermediate slepton or sneutrino to $l\nu\tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays through an intermediate scalar tau lepton or sneutrino to $\tau^+\tau^-\tilde{\chi}_1^0$ or $\nu\bar{\nu}\tilde{\chi}_1^0$.

**Tchi1n2I:** electroweak associated production of mass-degenerate charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ decays to $W^\pm + \tilde{\chi}_1^0$ and where $\tilde{\chi}_2^0$ decays 50% of the time to $Z + \tilde{\chi}_1^0$ and 50% of the time to $H + \tilde{\chi}_1^0$.

**Tchi1n12-GGM:** in the framework of General Gauge Mediation (GGM): electroweak pair and associated production of nearly mass-degenerate charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_1^0$, $\tilde{\chi}_1^0$, $\tilde{\chi}_1^0$, $\tilde{\chi}_1^0$ and $\tilde{\chi}_1^0$ production) where the $\tilde{\chi}_1^\pm$ decays exclusively to $W^\pm + \tilde{G}$, the $\tilde{\chi}_2^0$ decays to $Z/H + \tilde{G}$ and the $\tilde{\chi}_1^0$ decays to $\gamma/Z + \tilde{G}$. The branching ratios depend on the composition of the gauge eigenstates of the neutralinos in the GGM scenario.

**TwinoLSPBL:** Electroweak pair production of wino-like $\tilde{\chi}_1^\pm$ and $\tilde{\chi}_1^0$ (i.e. $\tilde{\chi}_1^\pm \tilde{\chi}_1^\pm$ and $\tilde{\chi}_1^0 \tilde{\chi}_1^0$). The $\tilde{\chi}_1^\pm$ can decay via bi-linear RPV into $Z\ell, H\ell$ or $W\nu$; the $\tilde{\chi}_1^0$ can decay into $Z\nu, H\nu$ or $W\ell$.

**Tn1n1A:** electroweak pair and associated production of nearly mass-degenerate Higgsino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_1^0$ and $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ and $\tilde{\chi}_2^0$ decay to $\tilde{\chi}_1^0$ plus soft radiation and where both of the $\tilde{\chi}_1^0$ decay to $H + \tilde{G}$.

**Tn1n1B:** electroweak pair and associated production of nearly mass-degenerate Higgsino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_1^0$ and $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ and $\tilde{\chi}_2^0$ decay to $\tilde{\chi}_1^0$ plus soft radiation and where the $\tilde{\chi}_1^0$ decays 50% of the time to $H + \tilde{G}$ and 50% of the time to $Z + \tilde{G}$.

**Tn1n1C:** electroweak pair and associated production of nearly mass-degenerate Higgsino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_1^0$ and $\tilde{\chi}_2^0$, where $\tilde{\chi}_1^\pm$ and $\tilde{\chi}_2^0$ decay to $\tilde{\chi}_1^0$ plus soft radiation and where both of the $\tilde{\chi}_1^0$ decay to $Z + \tilde{G}$.

**Tn1n1D:** electroweak pair and associated production of nearly mass-degenerate Higgsino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_1^0$, $\tilde{\chi}_2^0$.

**Tn1n1E:** electroweak pair and associated production of nearly mass-degenerate wino-like charginos $\tilde{\chi}_1^\pm$ and neutralinos $\tilde{\chi}_1^0$.

**Tn1n2A:** electroweak associated production of nearly mass-degenerate neutralinos $\tilde{\chi}_1^0$ and $\tilde{\chi}_2^0$, where the $\tilde{\chi}_2^0$ always decays to $\gamma + \tilde{G}$ and $\tilde{\chi}_1^0$ 50% of the time to $H + \tilde{G}$ and 50% of the time to $Z + \tilde{G}$.

**Tn2n3A:** electroweak associated production of mass-degenerate neutralinos $\tilde{\chi}_2^0$ and $\tilde{\chi}_3^0$, where $\tilde{\chi}_2^0$ and $\tilde{\chi}_3^0$ decay through intermediate sleptons to $l^+l^-\tilde{\chi}_1^0$ and where the slepton mass is 5%, 25%, 50%, 75% and 95% of the $\tilde{\chi}_2^0$ mass.

**Tn2n3B:** electroweak associated production of mass-degenerate neutralinos $\tilde{\chi}_2^0$ and $\tilde{\chi}_3^0$, where $\tilde{\chi}_2^0$ and $\tilde{\chi}_3^0$ decay through intermediate sleptons to $l^+l^-\tilde{\chi}_1^0$ and where $m_{\tilde{\chi}_2} = (m_{\tilde{\chi}_2^0} + m_{\tilde{\chi}_1^0})/2$.

**TWinoBinoA:** electroweak pair production of mass-degenerate wino-like doublet $(\tilde{\chi}_2^0, \tilde{\chi}_1^\pm)$ (including all pair-production mechanisms) decaying into a bino singlet $(\tilde{\chi}_1^0)$. Decays happen via Standard Model bosons, assumed to decay via hadrons.

**TWinoHinoA:** electroweak pair production of mass-degenerate wino-like doublet $(\tilde{\chi}_3^0, \tilde{\chi}_2^\pm)$ (including all possible pair-production mechanisms) decaying into a quasi-mass-degenerate Higgsino triplet $(\tilde{\chi}_1^0, \tilde{\chi}_2^0, \tilde{\chi}_1^\pm)$. Decays happen via Standard Model bosons, assumed to decay via hadrons.

**THinoBinoA:** electroweak pair production of quasi-mass-degenerate higgsino-like triplet $(\tilde{\chi}_2^0, \tilde{\chi}_3^0, \tilde{\chi}_1^\pm)$ (including all possible pair-production mechanisms) decaying into a bino singlet $(\tilde{\chi}_1^0)$. Decays happen via Standard Model bosons, assumed to decay via hadrons.

**THinoWinoA:** electroweak pair production of quasi-mass-degenerate higgsino-like triplet $(\tilde{\chi}_2^0, \tilde{\chi}_2^0, \tilde{\chi}_2^\pm)$ (including all possible pair-production mechanisms) decaying into a mass-degenerate wino doublet $(\tilde{\chi}_1^0, \tilde{\chi}_1^\pm)$. Decays happen via Standard Model bosons, assumed to decay via hadrons.

### $\tilde{\chi}_1^0$ (Lightest Neutralino) mass limit

$\tilde{\chi}_1^0$ is often assumed to be the lightest supersymmetric particle (LSP). See also the $\tilde{\chi}_2^0$, $\tilde{\chi}_3^0$, $\tilde{\chi}_4^0$ section below.

We have divided the $\tilde{\chi}_1^0$ listings below into five sections:

1) Accelerator limits for stable $\tilde{\chi}_1^0$.

2) Bounds on $\tilde{\chi}_1^0$ from dark matter searches,

3) $\tilde{\chi}_1^0 - \rho$ elastic cross section (spin-dependent, spin-independent interactions),

4) Other bounds on $\tilde{\chi}_1^0$ from astrophysics and cosmology, and

5) Unstable $\tilde{\chi}_1^0$ (Lightest Neutralino) mass limit.

### Accelerator limits for stable $\tilde{\chi}_1^0$

Unless otherwise stated, results in this section assume spectra, production rates, decay modes, and branching ratios as evaluated in the MSSM, with gaugino and sfermion mass unification at the GUT scale. These papers generally study production of $\tilde{\chi}_1^0 \tilde{\chi}_1^0$ ($i \ge 1, j \ge 2$), $\tilde{\chi}_1^+ \tilde{\chi}_1^-$, and (in the case of hadronic collisions) $\tilde{\chi}_1^+ \tilde{\chi}_1^0$ pairs. The mass limits on $\tilde{\chi}_1^0$ are either direct, or follow indirectly from the constraints set by the non-observation of $\tilde{\chi}_1^\pm$ and $\tilde{\chi}_2^0$ states on the gaugino and higgsino MSSM parameters $M_2$ and $\mu$. In some cases, information is used from the nonobservation of slepton decays.

Obsolete limits obtained from $e^+ e^-$ collisions up to $\sqrt{s}=184$ GeV have been removed from this compilation and can be found in the 2000 Edition (The European Physical Journal C15 1 (2000)) of this Review. $\Delta m = m_{\tilde{\chi}_2^0} - m_{\tilde{\chi}_1^0}$.

<table><thead><tr><th>VALUE (GeV)</th><th>CL<sub>L</sub></th><th>DOCUMENT ID</th><th>TECN.</th><th>COMMENT</th></tr></thead><tbody><tr><td>none 0.5-4.29</td><td>95</td><td>1 LEES</td><td>23C</td><td>B + charged track, RPV<br>B → $\tilde{\chi}_1^0 \rho, \lambda_{113}''$ of order<br>10<sup>-7</sup>–10<sup>-6</sup></td></tr><tr><td>&gt;150</td><td>95</td><td>2 AAD</td><td>22E</td><td>t$\tilde{\mu}_L$ production, RPV, $\tilde{\mu}_L$ →<br>$\mu \tilde{\chi}_1^0, \chi_L^{231} = 1, 200 \text{ GeV} &lt;$<br>m_{\tilde{\mu}_L} &lt; 600 \text{ GeV}$</td></tr><tr><td>none 125–175</td><td>95</td><td>3 TUMASYAN</td><td>22S</td><td>CMS<br>2 same-sign e or $\mu$, 3 or 4 leptons,<br>Tn1n1A, $m_{\tilde{G}} = 1$ GeV</td></tr><tr><td>none 125–415</td><td>95</td><td>3 TUMASYAN</td><td>22S</td><td>CMS<br>2 same-sign e or $\mu$, 3 or 4 leptons,<br>Tn1n1B, $m_{\tilde{G}} = 1$ GeV</td></tr></tbody></table>
<table><tbody><tr><td>none 100-625</td><td>95</td><td>3</td><td>TUMASYAN</td><td>22s</td><td>CMS</td><td>2 same-sign e or μ, 3 or 4 leptons, Tn1n1C, m<sub>G</sub> = 1 GeV</td></tr><tr><td>none 175-1025</td><td>95</td><td>4</td><td>TUMASYAN</td><td>22v</td><td>CMS</td><td>3, 4 b-tag jets or 2 large-radius jets, η<sub>T</sub>: Tn1n1A; m<sub>G</sub>=1 GeV</td></tr><tr><td>none 450-930</td><td>95</td><td>5</td><td>AAD</td><td>21AX</td><td>ATLS</td><td>jets + large-R jets + η<sub>T</sub>, Tn1n1C</td></tr><tr><td>none 200-320</td><td>95</td><td>6</td><td>AAD</td><td>21BF</td><td>ATLS</td><td>μ<sup>±</sup> + b-jets + many jets, Tn1n1D, RPV, λ<sup>"</sup>323 electroweakino decay, degenerate Higgsino triplet</td></tr><tr><td>none 200-370</td><td>95</td><td>6</td><td>AAD</td><td>21BF</td><td>ATLS</td><td>μ<sup>±</sup> + b-jets + many jets, Tn1n1E, RPV, λ<sup>"</sup>323 electroweakino decay, degenerate Wino doublet</td></tr><tr><td>&gt; 40</td><td>95</td><td>7</td><td>DREINER</td><td>09</td><td>THEO</td><td></td></tr><tr><td></td><td></td><td>8</td><td>ABBIENDI</td><td>04H</td><td>OPAL</td><td>all tanβ, Δm &gt;5 GeV, m<sub>0</sub> &gt;500 GeV, A<sub>0</sub> = 0</td></tr><tr><td>&gt; 42.4</td><td>95</td><td>9</td><td>HEISTER</td><td>04</td><td>ALEP</td><td>all tanβ, all Δm, all m<sub>0</sub></td></tr><tr><td>&gt; 39.2</td><td>95</td><td>10</td><td>ABDALLAH</td><td>03M</td><td>DLPH</td><td>all tanβ, m<sub>ν</sub> &gt;500 GeV</td></tr><tr><td>&gt; 46</td><td>95</td><td>11</td><td>ABDALLAH</td><td>03M</td><td>DLPH</td><td>all tanβ, all Δm, all m<sub>0</sub></td></tr><tr><td>&gt; 32.5</td><td>95</td><td>12</td><td>ACCIARRI</td><td>00d</td><td>L3</td><td>tanβ &gt; 0.7, Δm &gt; 3 GeV, all m<sub>0</sub></td></tr></tbody></table>

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

<table><tbody><tr><td>&gt; 24</td><td>13 AAD</td><td>14K</td><td>ATLS</td></tr><tr><td></td><td>14 CALIBBI</td><td>13</td><td>thermal relic abundance, MSSM particle content</td></tr></tbody></table>

¹ LEES 23c search in 398 fb⁻¹ of e⁺e⁻ annihilations at 10.58 GeV for SUSY in events with a tagged B meson and one and only one charged track that must be consistent with the hypothesis of being a proton. The results are interpreted in an RPV SUSY model, where a neutralino is produced in the decay of a B meson into a neutralino and a proton with the RPV coupling λ''<sub>113</sub>. A branching fraction upper limit is determined for the λ''<sub>113</sub> coupling, divided by the relevant squark mass squared as a function of the neutralino mass, see their figure 6. They also search for a new dark sector antibaryon that could be produced in decays of B mesons.

² AAD 22e searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for supersymmetry by measuring the yield asymmetry between events containing e⁻μ⁺ and those containing e⁺μ⁻. This was found in agreement with the standard model prediction of 1. Limits are set on the RPV production of tµ̄L events with t̄µ → µχ<sup>0</sup><sub>1</sub> for various values of λ''<sub>231</sub>, see their figures 6 and 7.

³ TUMASYAN 22s searched in 137 fb⁻¹ of pp collisions at √s = 13 TeV for evidence of electroweakino pair production in events with three or four leptons, with up to two hadronically decaying τ leptons, or two same-sign light leptons (e or μ). No significant excess above the Standard Model expectations is observed. Limits are set on the mass of χ<sup>0</sup><sub>2</sub> and χ<sup>±</sup><sub>1</sub> in the models Tchi1n2B (in flavory-democratic and tau-enriched or -dominated scenarios), Tchi1n2E, Tchi1n2F, see their Figures 16–20, and on the mass of the higgsino-triplet χ<sup>0</sup><sub>2</sub>, χ<sup>±</sup><sub>1</sub>, and χ<sup>0</sup><sub>1</sub> in the models Tn1n1A, Tn1n1B, and Tn1n1C, see their Figure 21.

⁴ TUMASYAN 22v searched in 137 fb⁻¹ of pp collisions at √s = 13 TeV for evidence of electroweakino pair production with decay to two Higgs bosons H, with H → bD, resulting either in 4 resolved b-jets or two large-radius jets, and large E<sub>T</sub>. No significant excess above the Standard Model expectations is observed. Limits are set on the mass of χ<sup>0</sup><sub>2</sub> and χ<sup>±</sup><sub>1</sub> in the models Tn1n1A, see their Figures 11 and 12, or in a model where higgsino-like nearly mass degenerate χ<sup>0</sup><sub>2</sub> and χ<sup>0</sup><sub>1</sub> are pair produced and each decay to H and a bino-like χ<sup>0</sup><sub>1</sub>, see their Figure 13. Limits are also set on the gluino mass in the model Tglu11, see their Figure 14.

⁵ AAD 21AX searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for pair production of electroweakinos decaying to the LSP via the emission of Standard Model bosons (Higgs, W, Z) decaying into hadrons. The final state in all cases characterised by the presence of E<sub>T</sub>, jets, and large-R jets tagged according to the boson of interest. Different assumptions (Higgsino, Wino, Bino) are made for the pair produced electroweakinos and for the LSP multipliet. No significant excess above the Standard Model predictions is observed. Limits are set on the electroweakino masses as a function of the model parameters (in particular m<sub>χ̄0</sub>). See Fig. 16.

⁶ AAD 21BF searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for pair production of gluinos, stops, electroweakinos decaying RPV either directly or indirectly via the LSP. The final state in all cases is one or two leptons, many jets (up to fifteen) and b-jets. Different models with different branching fractions of the gluino or stop follow from the assumptions on the nature of the electroweakinos. No significant excess above the Standard Model predictions is observed. Limits are set on the gluino, t<sub>1</sub>, electroweakino masses as a function of the χ<sup>0</sup><sub>1</sub> mass in several scenarios of gluino, stop and electroweakino pair production.

⁷ DREINER 09 show that in the general MSSM with non-universal gaugino masses there exists no model-independent laboratory bound on the mass of the lightest neutralino. An essentially massless χ<sup>0</sup><sub>1</sub> is allowed by the experimental and observational data, imposing some constraints on other MSSM parameters, including M<sub>2</sub>, μ and the slepton and squark masses.

⁸ ABBIENDI 04H search for charginos and neutralinos in events with acoplanar leptons-jets and multi-jet final states in the 192–209 GeV data, combined with the results on leptonic final states from ABBIENDI 04. The results hold for a scan over the parameter space covering the region 0 < M<sub>2</sub> < 5000 GeV, -1000 < μ < 1000 GeV and tanβ from 1 to 40. This limit supersedes ABBIENDI 00H.

⁹ HEISTER 04 data collected up to 209 GeV. Updates earlier analysis of selectrons from HEISTER 02E, includes a new analysis of charginos and neutralinos decaying into stau and uses results on charginos with initial state radiation from HEISTER 02J. The limit is based on the direct search for charginos and neutralinos, the constraints from the slepton search and the Higgs mass limits from HEISTER 02 using a top mass of 175 GeV, interpreted in a framework with universal gaugino and sfermion masses. Assuming the mixing in the stau sector to be negligible, the limit improves to 43.1 GeV. Under the assumption of MSUGRA with unification of the Higgs and sfermion masses, the limit improves to 50 GeV, and reaches 53 GeV for A<sub>0</sub> = 0. These limits include and update the results of BARATE 01.

¹⁰ ABDALLAH 03M uses data from √s = 192–208 GeV. A limit on the mass of χ<sup>0</sup><sub>1</sub> is derived from direct searches for neutralinos combined with the chargino search. Neutralinos are searched in the production of χ<sup>0</sup><sub>1</sub>χ<sup>0</sup><sub>2</sub>, χ<sup>0</sup><sub>1</sub>χ<sup>0</sup><sub>3</sub>, as well as χ<sup>0</sup><sub>2</sub>χ<sup>0</sup><sub>3</sub> and χ<sup>0</sup><sub>2</sub>χ<sup>0</sup><sub>4</sub> giving rise to cascade decays, and χ<sup>0</sup><sub>1</sub>χ<sup>0</sup><sub>2</sub> and χ<sup>0</sup><sub>1</sub>χ<sup>0</sup><sub>2</sub>, followed by the decay χ<sup>0</sup><sub>2</sub> → τ̄τ. The results hold for the parameter space defined by values of M<sub>2</sub> < 1 TeV, |μ| ≤ 2 TeV with the χ<sup>0</sup><sub>2</sub> as LSP. The limit is obtained for tanβ = 1 and large m<sub>0</sub>, where χ<sup>0</sup><sub>2</sub>χ<sup>0</sup><sub>4</sub> and chargino pair production are important. If the constraint from Higgs searches is also imposed, the limit improves to 49.0 GeV in the m<sub>h</sub><sup>max</sup> scenario with m<sub>t</sub>=174.3 GeV. These limits update the results of ABREU 00H.

¹¹ ABDALLAH 03M uses data from √s = 192–208 GeV. An indirect limit on the mass of χ<sup>0</sup><sub>1</sub> is derived by constraining the MSSM parameter space by the results from direct searches for neutralinos (including cascade decays and τ̄τ final states), for charginos (for all Δm<sub>+</sub>) and for sleptons, stop and bottom. The results hold for the full parameter space defined by values of M<sub>2</sub> < 1 TeV, |μ| ≤ 2 TeV with the χ<sup>0</sup><sub>1</sub> as LSP. Constraints from the Higgs search in the m<sub>h</sub><sup>max</sup> scenario assuming m<sub>t</sub>=174.3 GeV are included. The limit is obtained for tanβ ≥ 5 when stau mixing leads to mass degeneracy between τ̄<sub>1</sub> and χ<sup>0</sup><sub>2</sub> and the limit is based on χ<sup>0</sup><sub>2</sub> production followed by its decay to τ̄<sub>1</sub>τ. In the pathological scenario where m<sub>0</sub> and |μ| are large, so that the χ<sup>0</sup><sub>2</sub> production cross section is negligible, and where there is mixing in the stau sector but not in stop nor bottom, the limit is based on charginos with soft decay products and an ISR photon. The limit then degrades to 39 GeV. See Figs. 40–42 for the dependence of the limit on tanβ and m<sub>ν̄</sub>. These limits update the results of ABREU 00W.

¹² ACCIARRI 00D data collected at √s =189 GeV. The results hold over the full parameter space defined by 0.7 ≤ tanβ ≤ 60, 0 ≤ M<sub>2</sub> ≤ 2 TeV, m<sub>0</sub> ≤ 500 GeV, |μ| ≤ 2 TeV. The minimum mass limit is reached for tanβ=1 and large m<sub>0</sub>. The results of slepton searches from ACCIARRI 99W are used to help set constraints in the region of small m<sub>0</sub>. The limit improves to 48 GeV for m<sub>0</sub> ≥ 200 GeV and tanβ ≥ 10. See their Figs. 6–8 for the tanβ and m<sub>0</sub> dependence of the limits. Updates ACCIARRI 98F.

¹³ AAD 14k sets limits on the χ-nucleon spin-dependent and spin-independent cross sections out to m<sub>χ</sub> = 10 TeV.

¹⁴ CALIBBI 13 use the fact that if the relic abundance of χ<sup>0</sup><sub>1</sub> does not overclose the universe, scalar lepton and Higgsino masses must be relatively small. Using 8 TeV ATLAS constraints on the scalar tau mass and on invisible Higgs decays, they estimate a lower bound for the χ<sup>0</sup><sub>1</sub> mass.

## Bounds on $\tilde{\chi}_1^0$ from dark matter searches

These papers generally exclude regions in the M<sub>2</sub>–μ parameter plane assuming that χ<sup>0</sup><sub>1</sub> is the dominant form of dark matter in the galactic halo. These limits are based on the lack of detection in laboratory experiments, telescopes, or by the absence of a signal in underground neutrino detectors. The latter signal is expected if χ<sup>0</sup><sub>1</sub> accumulates in the Sun or the Earth and annihilates into high-energy ν̄s.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>• • •</td><td></td><td>We do not use the following data for averages, fits, limits, etc. • • •</td></tr></tbody></table>

<table><tbody><tr><td>1</td><td>ABE</td><td>23b</td><td>MGIC</td></tr><tr><td>2</td><td>FOSTER</td><td>23</td><td>FLAT</td></tr><tr><td>3</td><td>GUO</td><td>23A</td><td>ICCB</td></tr><tr><td>4</td><td>ABBASI</td><td>22B</td><td>ICCB</td></tr><tr><td>5</td><td>ABDALLA</td><td>22</td><td>HESS</td></tr><tr><td>6</td><td>ABDALLAH</td><td>21</td><td>HESS</td></tr><tr><td>7</td><td>ABAZAJIAN</td><td>20</td><td>FLAT</td></tr><tr><td>8</td><td>ABDALLAH</td><td>20</td><td>HESS</td></tr><tr><td>9</td><td>ABE</td><td>20G</td><td>SKAM</td></tr><tr><td>10</td><td>ALBERT</td><td>20G</td><td>HAWC</td></tr><tr><td>11</td><td>ALBERT</td><td>20A</td><td>ANTR</td></tr><tr><td>12</td><td>ALBERT</td><td>20C</td><td>ANIC</td></tr><tr><td>13</td><td>ALVAREZ</td><td>20G</td><td>FLAT</td></tr><tr><td>14</td><td>HOOF</td><td>20</td><td>FLAT</td></tr><tr><td>15</td><td>DI-MAURO</td><td>19</td><td>FLAT</td></tr><tr><td>16</td><td>JOHNSON</td><td>19</td><td>FLAT</td></tr><tr><td>17</td><td>LI</td><td>19D</td><td>FLAT</td></tr><tr><td>18</td><td>AHNEN</td><td>18</td><td>MGIC</td></tr><tr><td>19</td><td>ALBERT</td><td>18B</td><td>HAWC</td></tr><tr><td>20</td><td>ALBERT</td><td>18C</td><td>HAWC</td></tr><tr><td>21</td><td>AARTSEN</td><td>17</td><td>ICCB</td></tr><tr><td>22</td><td>AARTSEN</td><td>17A</td><td>ICCB</td></tr><tr><td>23</td><td>AARTSEN</td><td>17C</td><td>ICCB</td></tr><tr><td>24</td><td>ARCHAMBAU.</td><td>17</td><td>VRTS</td></tr><tr><td>25</td><td>ADRIAN-MAR.</td><td>16</td><td>ANTR</td></tr><tr><td>26</td><td>AHNEN</td><td>16</td><td>MGFL</td></tr><tr><td>27</td><td>AVRORIN</td><td>16</td><td>BAIK</td></tr><tr><td>28</td><td>CIRELLI</td><td>16</td><td>THEO</td></tr><tr><td>29</td><td>LEITE</td><td>16</td><td>THEO</td></tr><tr><td>30</td><td>ACKERMANN</td><td>15</td><td>FLAT</td></tr><tr><td>31</td><td>ACKERMANN</td><td>15A</td><td>FLAT</td></tr><tr><td>32</td><td>ACKERMANN</td><td>15B</td><td>FLAT</td></tr><tr><td>33</td><td>BUCKLEY</td><td>15</td><td>THEO</td></tr><tr><td>34</td><td>CHOI</td><td>15</td><td>SKAM</td></tr><tr><td>35</td><td>ALEKSIC</td><td>14</td><td>MGIC</td></tr><tr><td>36</td><td>AVRORIN</td><td>14</td><td>BAIK</td></tr><tr><td>37</td><td>AARTSEN</td><td>13C</td><td>ICCB</td></tr><tr><td>38</td><td>BERGSTROM</td><td>13</td><td>COSM</td></tr><tr><td>39</td><td>BOLIEV</td><td>13</td><td>BAKS</td></tr><tr><td>40</td><td>JIN</td><td>13</td><td>ASTR</td></tr></tbody></table>
37 KOPP 13 COSM

39 ACKERMANN 10 FLAT

40 ACHTERBERG 06 AMND

41 ACKERMANN 06 AMND

42 DEBOER 06 RVUE

43 DESAI 04 SKAM

43 AMBROSIO 99 MCRO

44 LOSECCO 95 RVUE

45 MORI 93 KAMI

46 BOTTINO 92 COSM

47 BOTTINO 91 RVUE

48 GELMINI 91 COSM

49 KAMIONKOW.91 RVUE

50 MORI 91B KAMI

none 4–15 GeV

1 ABE 23b sets limits on the dark matter annihilation cross section from line-like features in TeV gamma-rays in the direction of the Galactic center using the MAGIC stereoscopic telescope.

2 FOSTER 23 sets limits on the dark matter annihilation cross section from monochromatic gamma-rays in the inner Milky Way using 14 years of data from Fermi-LAT.

3 GUO 23A sets limits on the dark matter annihilation cross section from 10 years of IceCube muon-track data from 18 dwarf spheroidal galaxies.

4 ABBASI 22B presents 7 years of data from a search of neutrinos from dark matter annihilations in the sun using the DeepCore sub-array of IceCube. Annihilation cross section limits applies to dark matter masses between 5–100 GeV.

5 ABDALLA 22 uses gamma-ray observations in the Galactic center to constrain the dark matter annihilation cross section for annihilations into $WW$ and $\tau\tau$ for dark matter masses between 200 GeV to 70 TeV. This updates ABDALLAH 18.

6 ABDALLAH 21 places constraints on the dark matter annihilation cross section for annihilations into gamma-rays from the dwarf irregular galaxy WLM for masses between 0.15 to 10 TeV.

7 ABAZAJIAN 20 sets constraints on the dark matter annihilation from gamma-ray searches from Fermi LAT observations of the Galactic center.

8 ABDALLAH 20 places constraints on the dark matter annihilation cross section for annihilations into gamma-rays from Milky Way dwarf galaxy satellites for masses between 0.2 to 40 TeV.

9 ABE 20g is based on SuperKamiokande data taken from 1996 to 2016 searching for neutrinos produced from dark matter annihilations in the galactic center or halo. They place constraints on the dark matter-nucleon scattering cross section for dark matter masses between 1 GeV and 10 TeV.

10 ALBERT 20 sets limits on the annihilation cross section of dark matter with mass between 1 and 100 TeV from gamma-ray observations of the local dwarf spheroidal galaxies.

11 ALBERT 20A set limits on the dark matter annihilation cross section from neutrinos observations in the Galactic center using 11 years of ANTARES data.

12 ALBERT 20C set limits on the dark matter annihilation cross section from neutrinos observations in the Galactic center combining Antares and IceCube data.

13 ALVAREZ 20 set limits on the dark matter annihilation from gamma-ray searches from Fermi LAT observations in the directions of dwarf spheroidal galaxies.

14 HOOF 20 set limits on the dark matter annihilation from gamma-ray searches from Fermi LAT observations in the directions of dwarf spheroidal galaxies.

15 DI-MAURO 19 sets limits on the dark matter annihilation from gamma-ray searches in M31 and M33 galaxies using Fermi LAT data.

16 JOHNSON 19 sets limits on p-wave dark matter annihilations in the galactic center using Fermi data.

17 LI 19d sets limits on dark matter annihilation cross sections searching for line-like signals in the all-sky Fermi data.

18 AHNEN 18 uses observations of the dwarf satellite galaxy Ursa Major II to obtain upper limits on annihilation cross sections for dark matter in various channels for masses between 0.1–100 TeV.

19 ALBERT 18B sets limits on the annihilation cross section of dark matter with mass between 1 and 100 TeV from gamma-ray observations of the Andromeda galaxy.

20 ALBERT 18C sets limits on the spin-dependent coupling of dark matter to protons from dark matter annihilation in the Sun.

21 AARTSEN 17 is based on data collected during 327 days of detector live time with IceCube. They looked for interactions of $\nu$'s resulting from neutralino annihilations in the Earth over a background of atmospheric neutrinos and set 90% CL limits on the spin independent neutralino-proton cross section for neutralino masses in the range 10–10000 GeV.

22 AARTSEN 17A is based on data collected during 532 days of live time with the IceCube 86-string detector including the DeepCore sub-array. They looked for interactions of $\nu$'s from neutralino annihilations in the Sun over a background of atmospheric neutrinos and set 90% CL limits on the spin dependent neutralino-proton cross section for neutralino masses in the range 10–10000 GeV. This updates AARTSEN 16C.

23 AARTSEN 17c is based on 1005 days of running with the IceCube detector. They set a limit on the annihilation cross section for dark matter with masses between 10–1000 GeV annihilating in the Galactic center assuming an NFW profile. The limit is of $1.2 \times 10^{23}$ cm$^3$s$^{-1}$ in the $\tau^+\tau^-$ channel. Supercedes AARTSEN 15E.

24 ARCHAMBAULT 17 performs a joint statistical analysis of four dwarf galaxies with VERITAS looking for gamma-ray emission from neutralino annihilation. They set limits on the neutralino annihilation cross section.

25 ADRIAN-MARTINEZ 16 is based on data from the ANTARES neutrino telescope. They looked for interactions of $\nu$'s from neutralino annihilations in the Sun over a background of atmospheric neutrinos and set 90% CL limits on the muon neutrino flux. They also obtain limits on the spin dependent and spin independent neutralino-proton cross section for neutralino masses in the range 50 to 5,000 GeV. This updates ADRIAN-MARTINEZ 13.

26 AHNEN 16 combines 158 hours of Segue 1 observations with MAGIC 6 year observations of 15 dwarf satellite galaxies by Fermi-LAT to set limits on annihilation cross sections for dark matter masses between 10 GeV and 100 TeV.

27 AVRORIN 16 is based on 2.76 years with Lake Baikal neutrino telescope. They derive 90% upper limits on the annihilation cross section from dark matter annihilations in the Galactic center.

28 CIRELLI 16 and LEITE 16 derive bounds on the annihilation cross section from radio observations.

29 ACKERMANN 15 is based on 5.8 years of data with Fermi-LAT and search for monochromatic gamma-rays in the energy range of 0.2–500 GeV from dark matter annihilations. This updates ACKERMANN 13A.

30 ACKERMANN 15A is based on 50 months of data with Fermi-LAT and search for dark matter annihilation signals in the isotropic gamma-ray background as well as galactic subhalos in the energy range of a few GeV to a few tens of TeV.

31 ACKERMANN 15B is based on 6 years of data with Fermi-LAT observations of Milky Way dwarf spheroidal galaxies. Set limits on the annihilation cross section from $m_\chi = 2$ GeV to 10 TeV. This updates ACKERMANN 14.

32 BUCKLEY 15 is based on 5 years of Fermi-LAT data searching for dark matter annihilation signals from Large Magellanic Cloud.

33 CHOI 15 is based on 3903 days of SuperKamiokande data searching for neutrinos produced from dark matter annihilations in the sun. They place constraints on the dark matter-nucleon scattering cross section for dark matter masses between 4–200 GeV.

34 ALEKSIC 14 is based on almost 160 hours of observations of Segue 1 satellite dwarf galaxy using the MAGIC telescopes between 2011 and 2013. Sets limits on the annihilation cross section out to $m_\chi = 10$ TeV.

35 AVRORIN 14 is based on almost 2.76 years with Lake Baikal neutrino telescope. They derive 90% upper limits on the fluxes of muons and muon neutrinos from dark matter annihilations in the Sun.

36 AARTSEN 13c is based on data collected during 339.8 effective days with the IceCube 59-string detector. They looked for interactions of $\nu_\mu$'s from neutralino annihilations in nearby galaxies and galaxy clusters. They obtain limits on the neutralino annihilation cross section for neutralino masses in the range 30–100, 000 GeV.

37 BERGSTROM 13, JIN 13, and KOPP 13 derive limits on the mass and annihilation cross section using AMS-02 data. JIN 13 also sets a limit on the lifetime of the dark matter particle.

38 BOLIEV 13 is based on data collected during 24.12 years of live time with the Bakson Underground Scintillator Telescope. They looked for interactions of $\nu_\mu$'s from neutralino annihilations in the Sun over a background of atmospheric neutrinos and set 90% CL limits on the muon flux. They also obtain limits on the spin dependent and spin independent neutralino-proton cross section for neutralino masses in the range 10–1000 GeV.

39 ACKERMANN 10 place upper limits on the annihilation cross section with $b\bar{b}$ or $\mu^+\mu^-$ final states.

40 ACHTERBERG 06 is based on data collected during 421.9 effective days with the AMANDA detector. They looked for interactions of $\nu_\mu$'s from the centre of the Earth over a background of atmospheric neutrinos and set 90% CL limits on the muon flux. Their limit is compared with the muon flux expected from neutralino annihilations into $W^+W^-$ and $b\bar{b}$ at the centre of the Earth for MSSM parameters compatible with the relic dark matter density, see their Fig. 7.

41 ACKERMANN 06 is based on data collected during 143.7 days with the AMANDA-II detector. They looked for interactions of $\nu_\mu$'s from the Sun over a background of atmospheric neutrinos and set 90% CL limits on the muon flux. Their limit is compared with the muon flux expected from neutralino annihilations into $W^+W^-$ in the Sun for SUSY model parameters compatible with the relic dark matter density, see their Fig. 3.

42 DEBOER 06 interpret an excess of diffuse Galactic gamma rays observed with the EGRET satellite as originating from $\pi^0$ decays from the annihilation of neutralinos into quark jets. They analyze the corresponding parameter space in a supergravity inspired MSSM model with radiative electroweak symmetry breaking, see their Fig. 3 for the preferred region in the $(m_0, m_{1/2})$ plane of a scenario with large $\tan\beta$.

43 AMBROSIO 99 and DESAI 04 set new neutrino flux limits which can be used to limit the parameter space in supersymmetric models based on neutralino annihilation in the Sun and the Earth.

44 LOSECCO 95 reanalyzed the IMB data and places lower limit on $m_{\chi_1^0}$ of 18 GeV if the LSP is a photino and 10 GeV if the LSP is a higgsino based on LSP annihilation in the sun producing high-energy neutrinos and the limits on neutrino fluxes from the IMB detector.

45 MORI 93 excludes some region in $M_{2-\mu}$ parameter space depending on $\tan\beta$ and lightest scalar Higgs mass for neutralino dark matter $m_{\tilde{\chi}_1^0} > m_W$, using limits on upgoing muons produced by energetic neutrinos from neutralino annihilation in the Sun and the Earth.

46 BOTTINO 92 excludes some region $M_{2-\mu}$ parameter space assuming that the lightest neutralino is the dark matter, using upgoing muons at Kamiokande, direct searches by Ge detectors, and by LEP experiments. The analysis includes top radiative corrections on Higgs parameters and employs two different hypotheses for nucleon-Higgs coupling. Effects of rescaling in the local neutralino density according to the neutralino relic abundance are taken into account.

47 BOTTINO 91 excluded a region in $M_{2-\mu}$ plane using upgoing muon data from Kamioka experiment, assuming that the dark matter surrounding us is composed of neutralinos and that the Higgs boson is not too heavy.

48 GELMINI 91 exclude a region in $M_{2-\mu}$ plane using dark matter searches.

49 KAMIONKOWSKI 91 excludes a region in the $M_{2-\mu}$ plane using IMB limit on upgoing muons originated by energetic neutrinos from neutralino annihilation in the sun, assuming that the dark matter is composed of neutralinos and that $m_{H^0} \lesssim 50$ GeV. See Fig. 8 in the paper.

50 MORI 91b exclude a part of the region in the $M_{2-\mu}$ plane with $m_{\tilde{\chi}_1^0} \lesssim 80$ GeV using a limit on upgoing muons originated by energetic neutrinos from neutralino annihilation in the earth, assuming that the dark matter surrounding us is composed of neutralinos and that $m_{H^0} \lesssim 80$ GeV.

51 OLIVE 88 result assumes that photinos make up the dark matter in the galactic halo. Limit is based on annihilations in the sun and is due to an absence of high energy neutrinos detected in underground experiments. The limit is model dependent.

### $\tilde{\chi}_1^0-p$ elastic cross section

Experimental results on the $\tilde{\chi}_1^0-p$ elastic cross section are evaluated at $m_{\tilde{\chi}_1^0}=100$ GeV. The experimental results on the cross section are often mass dependent. Therefore, the mass and cross section results are also given where the limit is strongest, when appropriate. Results are quoted separately for spin-dependent interactions (based on an effective 4-Fermi Lagrangian of the form $\tilde{\chi}^\mu\gamma^5\tilde{\chi}\bar{\gamma}^\mu\gamma^5 q$) and spin-independent interactions ($\tilde{\chi}\bar{\chi}q$). For calculational details see GRIEST 88B, ELLIS 88D, BARIERI 89C, DREES 93B, ARROWITT 96, BERGSTROM 96, and BAER 97 in addition to the theory papers listed in the Tables. For a description of the theoretical assumptions and experimental techniques underlying most
of the listed papers, see the review on "Dark matter" in this "Review of Particle Physics," and references therein. Most of the following papers use galactic halo and nuclear interaction assumptions from (LEWIN 96).

Spin-dependent interactions

<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; 1.9 &times; 10<sup>-4</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>Xe</td></tr><tr><td>&lt; 3.3 &times; 10<sup>-4</sup></td><td>90</td><td>2 APRILE</td><td>23A XENT</td><td>Xe</td></tr><tr><td>&lt; 2 &times; 10<sup>-4</sup></td><td>90</td><td>3 HUANG</td><td>22 PNDX</td><td>Xe</td></tr><tr><td>&lt; 4 &times; 10<sup>-5</sup></td><td>90</td><td>4 AMOLE</td><td>19 PICO</td><td>C<sub>3</sub>F<sub>8</sub></td></tr><tr><td>&lt; 5 &times; 10<sup>-4</sup></td><td>90</td><td>5 APRILE</td><td>19A XE1T</td><td>Xe</td></tr><tr><td>&lt; 8 &times; 10<sup>-4</sup></td><td>90</td><td>6 AKERIB</td><td>17A LUX</td><td>Xe</td></tr><tr><td>&lt; 0.28</td><td>90</td><td>7 BATTAT</td><td>17 DRFT</td><td>CS<sub>2</sub>; CF<sub>4</sub></td></tr><tr><td>&lt; 0.027</td><td>90</td><td>8 BEHNKE</td><td>17 PICA</td><td>C<sub>4</sub>F<sub>10</sub></td></tr><tr><td>&lt; 5 &times; 10<sup>-4</sup></td><td>90</td><td>9 AMOLE</td><td>16 PICO</td><td>CF<sub>3</sub>I</td></tr><tr><td>&lt; 6.8 &times; 10<sup>-3</sup></td><td>90</td><td>10 APRILE</td><td>16B X100</td><td>Xe</td></tr><tr><td>&lt; 6.3 &times; 10<sup>-3</sup></td><td>90</td><td>11 FELIZARDO</td><td>14 SMPL</td><td>C<sub>2</sub>ClF<sub>5</sub></td></tr><tr><td>&lt; 0.01</td><td>90</td><td>12 AKIMOV</td><td>12 ZEP3</td><td>Xe</td></tr><tr><td>&lt; 7 &times; 10<sup>-3</sup></td><td></td><td>13 BEHNKE</td><td>12 COUP</td><td>CF<sub>3</sub>I</td></tr><tr><td>&lt; 8.5 &times; 10<sup>-3</sup></td><td></td><td>14 FELIZARDO</td><td>12 SMPL</td><td>C<sub>2</sub>ClF<sub>5</sub></td></tr><tr><td>&lt; 0.016</td><td>90</td><td>15 KIM</td><td>12 KIMS</td><td>CsI</td></tr><tr><td>5 &times; 10<sup>-10</sup> to 10<sup>-5</sup></td><td>95</td><td>16 BUCHMUEL...</td><td>11B THEO</td><td></td></tr><tr><td>&lt; 1</td><td>95</td><td>17 ANGLE</td><td>08A XE10</td><td>Xe</td></tr><tr><td>&lt; 0.055</td><td></td><td>18 BEDNYAKOV</td><td>08 HDMS</td><td>Ge</td></tr><tr><td>&lt; 0.33</td><td>90</td><td>19 BEHNKE</td><td>08 COUP</td><td>CF<sub>3</sub>I</td></tr><tr><td>&lt; 5</td><td></td><td>20 AKERIB</td><td>06 CDMS</td><td>Ge</td></tr><tr><td>&lt; 2</td><td></td><td>21 SHIMIZU</td><td>06A CNTR</td><td>CaF<sub>2</sub></td></tr><tr><td>&lt; 0.4</td><td></td><td>22 ALNER</td><td>05 NAIA</td><td>Nal Spin Dep.</td></tr><tr><td>&lt; 2</td><td></td><td>23 BARNABE-HE.05</td><td>05 PICA</td><td>C</td></tr><tr><td>2 &times; 10<sup>-11</sup> to 1 &times; 10<sup>-4</sup></td><td></td><td>24 ELLIS</td><td>04 THEO</td><td>&mu; &gt; 0</td></tr><tr><td>&lt; 0.8</td><td></td><td>25 AHMED</td><td>03 NAIA</td><td>Nal Spin Dep.</td></tr><tr><td>&lt; 40</td><td></td><td>26 TAKEDA</td><td>03 BOLO</td><td>NaF Spin Dep.</td></tr><tr><td>&lt; 10</td><td></td><td>27 ANGLOHER</td><td>02 CRES</td><td>Saphire</td></tr><tr><td>8 &times; 10<sup>-7</sup> to 2 &times; 10<sup>-5</sup></td><td></td><td>28 ELLIS</td><td>01C THEO</td><td>&tan;&beta; &le; 10</td></tr><tr><td>&lt; 3.8</td><td></td><td>29 BERNABEI</td><td>00D DAMA</td><td>Xe</td></tr><tr><td>&lt; 0.8</td><td></td><td>SPOONER</td><td>00 UKDM</td><td>Nal</td></tr><tr><td>&lt; 4.8</td><td></td><td>30 BELLI</td><td>99C DAMA</td><td>F</td></tr><tr><td>&lt;100</td><td></td><td>31 OOTANI</td><td>99 BOLO</td><td>LiF</td></tr><tr><td>&lt; 0.6</td><td></td><td>BERNABEI</td><td>98C DAMA</td><td>Xe</td></tr><tr><td>&lt; 5</td><td></td><td>30 BERNABEI</td><td>97 DAMA</td><td>F</td></tr></tbody></table>

1. The strongest upper limit is $4.2 \times 10^{-5}$ pb at 32 GeV. The limit for scattering on neutrons is $4 \times 10^{-6}$ pb at 100 GeV and is $1.5 \times 10^{-6}$ pb at 30 GeV.

2. The strongest upper limit is $1.4 \times 10^{-4}$ pb at 28 GeV. The limit for scattering on neutrons is $1.1 \times 10^{-5}$ pb at 100 GeV and is $4.3 \times 10^{-6}$ pb at 28 GeV.

3. The strongest limit is $< 1.7 \times 10^{-4}$ pb at $m_{\chi} = 40$ GeV. This updates FU 17 and XIA 19A.

4. The strongest limit is $< 3.2 \times 10^{-5}$ pb at $m_{\chi} = 25$ GeV. This updates AMOLE 17.

5. The strongest limit is $< 2 \times 10^{-4}$ pb at $m_{\chi} = 30$ GeV. For scatterings on neutrons, the strongest limit is $< 6.3 \times 10^{-6}$ at $m_{\chi} = 30$ GeV.

6. The strongest limit is $5 \times 10^{-4}$ pb at $m_{\chi} = 35$ GeV. The limit for scattering on neutrons is $3 \times 10^{-5}$ pb at 100 GeV and is $1.6 \times 10^{-5}$ pb at 35 GeV. This updates AKERIB 16A.

7. Directional recoil detector. This updates DAW 12.

8. This result updates ARCHAMBAULT 12. The strongest limit is 0.013 pb at $m_{\chi} = 20$ GeV.

9. The strongest limit is $5 \times 10^{-4}$ pb at $m_{\chi} = 80$ GeV.

10. The strongest limit is $5.2 \times 10^{-3}$ pb at 50 GeV. The limit for scattering on neutrons is $2.8 \times 10^{-4}$ pb at 100 GeV and the strongest limit is $2.0 \times 10^{-4}$ pb at 50 GeV. This updates APRILE 13.

11. The strongest limit is 0.0043 pb and occurs at $m_{\chi} = 35$ GeV. FELIZARDO 14 also presents limits for the scattering on neutrons. At $m_{\chi} = 100$ GeV, the upper limit is 0.13 pb and the strongest limit is 0.066 pb at $m_{\chi} = 35$ GeV.

12. This result updates LEBEDENKO 09A. The strongest limit is $8 \times 10^{-3}$ pb at $m_{\chi} = 50$ GeV. Limit applies to the neutralino neutron elastic cross section.

13. The strongest limit is $6 \times 10^{-3}$ at $m_{\chi} = 60$ GeV.

14. The strongest limit is $5.7 \times 10^{-3}$ at $m_{\chi} = 35$ GeV.

15. This result updates LEE 07A. The strongest limit is at $m_{\chi} = 80$ GeV.

16. Predictions for the spin-dependent elastic cross section based on a frequentist approach to electroweak observables in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

17. The strongest limit is 0.6 pb and occurs at $m_{\chi} = 30$ GeV. The limit for scattering on neutrons is 0.01 pb at $m_{\chi} = 100$ GeV, and the strongest limit is 0.0045 pb at $m_{\chi} = 30$ GeV.

18. Limit applies to neutron elastic cross section.

19. The strongest upper limit is 0.25 pb and occurs at $m_{\chi} \simeq 40$ GeV.

20. The strongest upper limit is 4 pb and occurs at $m_{\chi} \simeq 60$ GeV. The limit on the neutron spin-dependent elastic cross section is 0.07 pb. This latter limit is improved in AHMED 09, where a limit of 0.02 pb is obtained at $m_{\chi} = 100$ GeV. The strongest limit in AHMED 09 is 0.018 pb and occurs at $m_{\chi} = 60$ GeV.

21. The strongest upper limit is 1.2 pb and occurs at $m_{\chi} \simeq 40$ GeV. The limit on the neutron spin-dependent cross section is 35 pb.

22. The strongest upper limit is 0.35 pb and occurs at $m_{\chi} \simeq 60$ GeV.

23. The strongest upper limit is 1.2 pb and occurs $m_{\chi} \simeq 30$ GeV.

24. ELLIS 04 calculates the $\chi_p$ elastic scattering cross section in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry, but without universal scalar masses. In the case of universal squark and slepton masses, but non-universal Higgs masses, the limit becomes $2 \times 10^{-4}$, see ELLIS 03E.

25. The strongest upper limit is 0.75 pb and occurs at $m_{\chi} \simeq 70$ GeV.

26. The strongest upper limit is 30 pb and occurs at $m_{\chi} \simeq 20$ GeV.

27. The strongest upper limit is 8 pb and occurs at $m_{\chi} \simeq 30$ GeV.

28. ELLIS 01C calculates the $\chi_p$ elastic scattering cross section in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry. In models with nonuniversal Higgs masses, the upper limit to the cross section is $6 \times 10^{-4}$.

29. The strongest upper limit is 3 pb and occurs at $m_{\chi} \simeq 60$ GeV. The limits are for inelastic scattering $X^0 + 129X_e \rightarrow X^0 + 129X_e^*$ (39.58 keV).

30. The strongest upper limit is 4.4 pb and occurs at $m_{\chi} \simeq 60$ GeV.

31. The strongest upper limit is about 35 pb and occurs at $m_{\chi} \simeq 15$ GeV.

Spin-independent interactions

<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>-11</sup></td><td>90</td><td>1 AALBERS</td><td>23 LZ</td><td>Xe</td></tr><tr><td>&lt; 6.1 &times; 10<sup>-11</sup></td><td>90</td><td>2 APRILE</td><td>23A XENT</td><td>Xe</td></tr><tr><td>&lt; 6.5 &times; 10<sup>-11</sup></td><td>90</td><td>3 MENG</td><td>21B PNDX</td><td>Xe</td></tr><tr><td>&lt; 5 &times; 10<sup>-10</sup></td><td>90</td><td>4 WANG</td><td>20G PNDX</td><td>Xe</td></tr><tr><td>&lt; 2.5 &times; 10<sup>-8</sup></td><td>90</td><td>5 ABE</td><td>19 XMAS</td><td>Xe</td></tr><tr><td>&lt; 3.9 &times; 10<sup>-9</sup></td><td>90</td><td>6 AJAJ</td><td>19 DEAP</td><td>Ar</td></tr><tr><td>&lt; 2 &times; 10<sup>-8</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; 2.25 &times; 10<sup>-6</sup></td><td>90</td><td>8 ADHIKARI</td><td>18 C100</td><td>Nal</td></tr><tr><td>&lt; 1.14 &times; 10<sup>-8</sup></td><td>90</td><td>9 AGNES</td><td>18A DS50</td><td>Ar</td></tr><tr><td>&lt; 1.6 &times; 10<sup>-8</sup></td><td>90</td><td>10 AGNESE</td><td>18A CDMS</td><td>Ge</td></tr><tr><td>&lt; 9 &times; 10<sup>-11</sup></td><td>90</td><td>11 APRILE</td><td>18 XE1T</td><td>Xe</td></tr><tr><td>&lt; 1.8 &times; 10<sup>-10</sup></td><td>90</td><td>12 AKERIB</td><td>17 LUX</td><td>Xe</td></tr><tr><td>&lt; 1.5 &times; 10<sup>-9</sup></td><td>90</td><td>13 APRILE</td><td>16B X100</td><td>Xe</td></tr><tr><td>&lt; 1.5 &times; 10<sup>-9</sup></td><td>90</td><td>14 AKERIB</td><td>14 LUX</td><td>Xe</td></tr><tr><td>10<sup>-11</sup> &times; 10<sup>-7</sup></td><td>95</td><td>15 BUCHMUEL...</td><td>14A THEO</td><td></td></tr><tr><td>&lt; 4.6 &times; 10<sup>-6</sup></td><td>95</td><td>16 FELIZARDO</td><td>14 SMPL</td><td>C<sub>2</sub>ClF<sub>5</sub></td></tr><tr><td>10<sup>-11</sup> &times; 10<sup>-8</sup></td><td>95</td><td>17 ROSZKOWSKI</td><td>14 THEO</td><td></td></tr><tr><td>&lt; 2.2 &times; 10<sup>-6</sup></td><td>95</td><td>18 AGNESE</td><td>13 CDMS</td><td>Si</td></tr><tr><td>&lt; 5 &times; 10<sup>-8</sup></td><td>90</td><td>19 AKIMOV</td><td>12 ZEP3</td><td>Xe</td></tr><tr><td>1.6 &times; 10<sup>-6</sup>; 3.7 &times; 10<sup>-5</sup></td><td></td><td>20 ANGLOHER</td><td>12 CRES</td><td>CaWO<sub>4</sub></td></tr><tr><td>3 &times; 10<sup>-12</sup> to 3 &times; 10<sup>-9</sup></td><td>95</td><td>21 BECHTLE</td><td>12 THEO</td><td></td></tr><tr><td>&lt; 1.6 &times; 10<sup>-7</sup></td><td></td><td>22 BEHNKE</td><td>12 COUP</td><td>CF<sub>3</sub>I</td></tr><tr><td>&lt; 2.3 &times; 10<sup>-7</sup></td><td>90</td><td>23 KIM</td><td>12 KIMS</td><td>CsI</td></tr><tr><td>&lt; 3.3 &times; 10<sup>-8</sup></td><td>90</td><td>24 AHMED</td><td>11A</td><td>Ge</td></tr><tr><td>&lt; 4.4 &times; 10<sup>-8</sup></td><td>90</td><td>25 ARMENGAUD</td><td>11 EDE2</td><td>Ge</td></tr><tr><td>&lt; 1 &times; 10<sup>-7</sup></td><td>90</td><td>26 ANGLE</td><td>08 XE10</td><td>Xe</td></tr><tr><td>&lt; 1 &times; 10<sup>-6</sup></td><td>90</td><td>BENETTI</td><td>08 WARP</td><td>Ar</td></tr><tr><td>&lt; 7.5 &times; 10<sup>-7</sup></td><td>90</td><td>27 ALNER</td><td>07A ZEP2</td><td>Xe</td></tr><tr><td>&lt; 2 &times; 10<sup>-7</sup></td><td></td><td>28 AKERIB</td><td>06A CDMS</td><td>Ge</td></tr><tr><td>&lt; 90 &times; 10<sup>-7</sup></td><td></td><td>ALNER</td><td>05 NAIA</td><td>Nal Spin Indep.</td></tr><tr><td>&lt;12 &times; 10<sup>-7</sup></td><td></td><td>29 ALNER</td><td>05A ZEPL</td><td></td></tr><tr><td>&lt;14 &times; 10<sup>-7</sup></td><td></td><td>SANGLARD</td><td>05 EDEL</td><td>Ge</td></tr><tr><td>&lt; 4 &times; 10<sup>-7</sup></td><td></td><td>30 AKERIB</td><td>04 CDMS</td><td>Ge</td></tr><tr><td>2 &times; 10<sup>-11</sup> to 1.5 &times; 10<sup>-7</sup></td><td>95</td><td>31 BALTZ</td><td>04 THEO</td><td></td></tr><tr><td>2 &times; 10<sup>-11</sup> to 8 &times; 10<sup>-6</sup></td><td></td><td>32,33 ELLIS</td><td>04 THEO</td><td>&mu; &gt; 0</td></tr><tr><td>&lt; 5 &times; 10<sup>-8</sup></td><td></td><td>34 PIERCE</td><td>04A THEO</td><td></td></tr><tr><td>&lt; 2 &times; 10<sup>-5</sup></td><td></td><td>35 AHMED</td><td>03 NAIA</td><td>Nal Spin Indep.</td></tr><tr><td>&lt; 3 &times; 10<sup>-6</sup></td><td></td><td>36 AKERIB</td><td>03 CDMS</td><td>Ge</td></tr><tr><td>2 &times; 10<sup>-13</sup> to 2 &times; 10<sup>-7</sup></td><td></td><td>37 BAER</td><td>03A THEO</td><td></td></tr><tr><td>&lt; 1.4 &times; 10<sup>-5</sup></td><td></td><td>38 KLPDOR-K...</td><td>03 HDMS</td><td>Ge</td></tr><tr><td>&lt; 6 &times; 10<sup>-6</sup></td><td></td><td>39 ABRAMS</td><td>02 CDMS</td><td>Ge</td></tr><tr><td>1 &times; 10<sup>-12</sup> to 7 &times; 10<sup>-6</sup></td><td></td><td>32 KIM</td><td>02B THEO</td><td></td></tr><tr><td>&lt; 3 &times; 10<sup>-5</sup></td><td></td><td>40 MORALES</td><td>02B CSME</td><td>Ge</td></tr><tr><td>&lt; 1 &times; 10<sup>-5</sup></td><td></td><td>41 MORALES</td><td>02C IGEX</td><td>Ge</td></tr><tr><td>&lt; 1 &times; 10<sup>-6</sup></td><td></td><td>BALTZ</td><td>01 THEO</td><td></td></tr><tr><td>&lt; 3 &times; 10<sup>-5</sup></td><td></td><td>42 BAUDIS</td><td>01 HDMS</td><td>Ge</td></tr><tr><td>&lt; 7 &times; 10<sup>-6</sup></td><td></td><td>43 BOTTINO</td><td>01 THEO</td><td></td></tr><tr><td>&lt; 1 &times; 10<sup>-8</sup></td><td></td><td>44 CORSETTI</td><td>01 THEO</td><td>&tan;&beta; &le; 25</td></tr><tr><td>5 &times; 10<sup>-10</sup> to 1.5 &times; 10<sup>-8</sup></td><td></td><td>45 ELLIS</td><td>01C THEO</td><td>&tan;&beta; &le; 10</td></tr><tr><td>&lt; 4 &times; 10<sup>-6</sup></td><td></td><td>44 GOMEZ</td><td>01 THEO</td><td></td></tr><tr><td>2 &times; 10<sup>-10</sup> to 1 &times; 10<sup>-7</sup></td><td></td><td>44 LAHANAS</td><td>01 THEO</td><td></td></tr><tr><td>&lt; 3 &times; 10<sup>-6</sup></td><td></td><td>ABUSAIDI</td><td>00 CDMS</td><td>Ge, Si</td></tr><tr><td>&lt; 6 &times; 10<sup>-7</sup></td><td></td><td>46 ACCOMANDO</td><td>00 THEO</td><td></td></tr><tr><td>2.5 &times; 10<sup>-9</sup> to 3.5 &times; 10<sup>-8</sup></td><td></td><td>47 BERNABEI</td><td>00 DAMA</td><td>Nal</td></tr><tr><td>&lt; 1.5 &times; 10<sup>-5</sup></td><td></td><td>48 FENG</td><td>00 THEO</td><td>&tan;&beta;=10</td></tr><tr><td>&lt; 4 &times; 10<sup>-5</sup></td><td></td><td>MORALES</td><td>00 IGEX</td><td>Ge</td></tr><tr><td>&lt; 7 &times; 10<sup>-6</sup></td><td></td><td>SPOONER</td><td>00 UKDM</td><td>Nal</td></tr><tr><td>&lt; 7 &times; 10<sup>-6</sup></td><td></td><td>BAUDIS</td><td>99 HDMO</td><td>76Ge</td></tr><tr><td>&lt; 7 &times; 10<sup>-6</sup></td><td></td><td>BERNABEI</td><td>98 DAMA</td><td>Xe</td></tr></tbody></table>

1. The strongest upper limit is $9.2 \times 10^{-12}$ pb at 36 GeV.

2. The strongest upper limit is $2.6 \times 10^{-11}$ pb at 28 GeV.

3. Commissioning Run for PandaX-4T. The strongest limit is $3.8 \times 10^{-11}$ pb at $m_{\chi} = 40$ GeV.

4. WANG 20G strongest limit is $2.2 \times 10^{-10}$ pb at 30 GeV using 132 ton-day full exposure of PandaX-II. This updates CUI 17A, though the results here provide weaker constraints.

5. The strongest upper limit is $2.2 \times 10^{-8}$ pb at 60 GeV.

6. This updates AMAUDRUZ 18.
# Searches Particle Listings
## Supersymmetric Particle Searches

7 This updates AMOLE 16.

8 The strongest limit is $2.05 \times 10^{-6}$ at $m = 60$ GeV.

9 The strongest limit is $1.09 \times 10^{-8}$ pb at $m_\chi = 126$ GeV. This updates AGNES 15.

10 The strongest limit is $1.0 \times 10^{-8}$ pb at $m_\chi = 46$ GeV. This updates AGNESE 15b.

11 Based on 278.8 days of data collection. The strongest limit is $4.1 \times 10^{-11}$ pb at $m_\chi = 30$ GeV. This updates APRILE 17g.

12 AKERIB 17. The strongest limit is $1.1 \times 10^{-10}$ pb at 50 GeV. This updates AKERIB 16.

13 The strongest limit is $1.1 \times 10^{-9}$ pb at 50 GeV. This updates APRILE 12.

14 The strongest upper limit is $7.6 \times 10^{-10}$ at $m_\chi = 33$ GeV.

15 Predictions for the spin-independent elastic cross section based on a frequentist approach to electroweak observables in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using the $20 \text{ fb}^{-1}$ 8 TeV and the $5 \text{ fb}^{-1}$ 7 TeV LHC data and the LUX data.

16 The strongest limit is $3.6 \times 10^{-6}$ pb and occurs at $m_\chi = 35$ GeV. Felizardo 2014 updates Felizardo 2012.

17 Predictions for the spin-independent elastic cross section based on a Bayesian approach to electroweak observables in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using the $20 \text{ fb}^{-1}$ LHC data and LUX.

18 AGNESE 13 presents 90% CL limits on the elastic cross section for masses in the range 7-100 GeV using the Si based detector. The strongest upper limit is $1.8 \times 10^{-6}$ pb at $m_\chi = 50$ GeV. This limit is improved to $7 \times 10^{-7}$ pb in AGNESE 13A.

19 This result updates LEBEDENKO 09. The strongest limit is $3.9 \times 10^{-8}$ pb at $m_\chi = 52$ GeV.

20 ANGLOHER 12 presents results of 730 kg days from the CRESST-II dark matter detector. They find two maxima in the likelihood function corresponding to best fit WIMP masses of 25.3 and 11.6 GeV with elastic cross sections of $1.6 \times 10^{-6}$ and $3.7 \times 10^{-5}$ pb respectively, see their Table 4. The statistical significance is more than $4\sigma$. ANGLOHER 12 updates ANGLOHER 09.

21 Predictions for the spin-independent elastic cross section based on a frequentist approach to electroweak observables in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using the $5 \text{ fb}^{-1}$ LHC data and XENON100.

22 The strongest limit is $1.4 \times 10^{-7}$ at $m_\chi = 60$ GeV.

23 This result updates LEE 07A. The strongest limit is $2.1 \times 10^{-7}$ at $m_\chi = 70$ GeV.

24 AHMED 11A gives combined results from CDMS and EDELWEISS. The strongest limit is at $m_\chi = 90$ GeV.

25 ARMENGAUD 11 updates result of ARMENGAUD 10. Strongest limit at $m_\chi = 85$ GeV.

26 The strongest upper limit is $5.1 \times 10^{-8}$ pb and occurs at $m_\chi \approx 30$ GeV. The values quoted here are based on the analysis performed in ANGLE 08 with the update from SORENSEN 09.

27 The strongest upper limit is $6.6 \times 10^{-7}$ pb and occurs at $m_\chi \approx 65$ GeV.

28 AKERIB 06A updates the results of AKERIB 05. The strongest upper limit is $1.6 \times 10^{-7}$ pb and occurs at $m_\chi \approx 60$ GeV.

29 The strongest upper limit is also close to $1.0 \times 10^{-6}$ pb and occurs at $m_\chi \approx 70$ GeV. BENOIT 06 claim that the discrimination power of ZEPLIN-I measurement (ALNER 05A) is not reliable enough to obtain a limit better than $1 \times 10^{-3}$ pb. However, SMITH 06 do not agree with the criticisms of BENOIT 06.

30 AKERIB 04 is incompatible with BERNABEI 00 most likely value, under the assumption of standard WIMP-halo interactions. The strongest upper limit is $4 \times 10^{-7}$ pb and occurs at $m_\chi \approx 60$ GeV.

31 Predictions for the spin-independent elastic cross section in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

32 KIM 02 and ELLIS 04 calculate the $\chi p$ elastic scattering cross section in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry, but without universal scalar masses.

33 In the case of universal squark and slepton masses, but non-universal Higgs masses, the limit becomes $2 \times 10^{-6}$ ($2 \times 10^{-11}$ when constraint from the BNL g-2 experiment are included), see ELLIS 03E. ELLIS 05 display the sensitivity of the elastic scattering cross section to the $\pi$-Nucleon $\Sigma$ term.

34 PIERCE 04A calculates the $\chi p$ elastic scattering cross section in the framework of models with very heavy scalar masses. See Fig. 2 of the paper.

35 The strongest upper limit is $1.8 \times 10^{-5}$ pb and occurs at $m_\chi \approx 80$ GeV.

36 Under the assumption of standard WIMP-halo interactions, Akerib 03 is incompatible with BERNABEI 00 most likely value at the 99.98% CL. See Fig. 4.

37 BAER 03A calculates the $\chi p$ elastic scattering cross section in several models including the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

38 The strongest upper limit is $7 \times 10^{-6}$ pb and occurs at $m_\chi \approx 30$ GeV.

39 ABRAMS 02 is incompatible with the DAMA most likely value at the 99.9% CL. The strongest upper limit is $3 \times 10^{-6}$ pb and occurs at $m_\chi \approx 30$ GeV.

40 The strongest upper limit is $2 \times 10^{-5}$ pb and occurs at $m_\chi \approx 40$ GeV.

41 The strongest upper limit is $7 \times 10^{-6}$ pb and occurs at $m_\chi \approx 46$ GeV.

42 The strongest upper limit is $1.8 \times 10^{-5}$ pb and occurs at $m_\chi \approx 32$ GeV.

43 BOTTINO 01 calculates the $\chi p$ elastic scattering cross section in the framework of the following supersymmetric models: $N=1$ supergravity with the radiative breaking of the electroweak gauge symmetry, $N=1$ supergravity with nonuniversal scalar masses and an effective MSSM model at the electroweak scale.

44 Calculates the $\chi p$ elastic scattering cross section in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

45 ELLIS 01C calculates the $\chi p$ elastic scattering cross section in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry. ELLIS 02B find a range $2 \times 10^{-8} - 1.5 \times 10^{-7}$ at $\tan\beta=50$. In models with nonuniversal Higgs masses, the upper limit to the cross section is $4 \times 10^{-7}$.

46 ACCOMANDO 00 calculates the $\chi p$ elastic scattering cross section in the framework of minimal $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry. The limit is relaxed by at least an order of magnitude when models with nonuniversal scalar masses are considered. A subset of the authors in ARNOWITT 02 updated the limit to $< 9 \times 10^{-8}$ ($\tan\beta < 55$).

47 BERNABEI 00 search for annual modulation of the WIMP signal. The data favor the hypothesis of annual modulation at $4\sigma$ and are consistent, for a particular model framework quoted there, with $m_\chi^0 = 44 \pm 12/9$ GeV and a spin-independent $\chi^0$-proton cross section of $(5.4 \pm 1.0) \times 10^{-6}$ pb. See also BERNABEI 01 and BERNABEI 00c.

48 FENG 00 calculate the $\chi p$ elastic scattering cross section in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry with a particular emphasis on focus point models. At $\tan\beta=50$, the range is $8 \times 10^{-8} - 4 \times 10^{-7}$.

## Other bounds on $\tilde{\chi}_1^0$ from astrophysics and cosmology

Most of these papers generally exclude regions in the $M_2-\mu$ parameter plane by requiring that the $\tilde{\chi}_1^0$ contribution to the overall cosmological density is less than some maximal value to avoid overclosure of the Universe. Those not based on the cosmological density are indicated. Many of these papers also include LEP and/or other bounds.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;46 GeV</td><td>1 ELLIS</td><td>00</td><td>RVUE</td></tr><tr><td>&gt; 18 GeV</td><td>1</td><td></td><td>• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>&gt; 6 GeV</td><td>2 ATHRON</td><td>17b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>3 BECHTLE</td><td>16</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>4 BAGNASCHI</td><td>15</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 BUCHMUEL...</td><td>14</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>6 BUCHMUEL...</td><td>14A</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>7 ROSZKOWSKI</td><td>14</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>8 CABRERA</td><td>13</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>9 ELLIS</td><td>13b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>8 STREGE</td><td>13</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 AKULA</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 ARBEY</td><td>12A</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 BAER</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>10 BALAZS</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>11 BECHTLE</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>12 BESKIDT</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>13 BOTTINO</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 BUCHMUEL...</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 CAO</td><td>12A</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 ELLIS</td><td>12b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>14 FENG</td><td>12b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>5 KADASTIK</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>10 STREGE</td><td>12</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>15 BUCHMUEL...</td><td>11</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>16 ROSZKOWSKI</td><td>11</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>17 ELLIS</td><td>10</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>18 BUCHMUEL...</td><td>09</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>19 DREINER</td><td>09</td><td>THEO</td></tr><tr><td>&gt; 6 GeV</td><td>20 BUCHMUEL...</td><td>08</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>16 ELLIS</td><td>08</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>21 CALIBBI</td><td>07</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>22 ELLIS</td><td>07</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>23 ALLANACH</td><td>06</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>24 DE-AUSTRI</td><td>06</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>16 BAER</td><td>05</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>25 BALTZ</td><td>04</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>13,26 BELANGER</td><td>04</td><td>THEO</td></tr><tr><td>&gt; 6 GeV</td><td>27 ELLIS</td><td>04b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>28 PIERCE</td><td>04A</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>29 BAER</td><td>03</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>13 BOTTINO</td><td>03</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>29 CHATTOPAD...</td><td>03</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>30 ELLIS</td><td>03</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>16 ELLIS</td><td>03b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>29 ELLIS</td><td>03c</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>29 LAHANAS</td><td>03</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>31 LAHANAS</td><td>02</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>32 BARGER</td><td>01c</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>33 ELLIS</td><td>01b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>30 BOEHM</td><td>00b</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>34 FENG</td><td>00</td><td>COSM</td></tr><tr><td>&gt; 6 GeV</td><td>35 ELLIS</td><td>98b</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>36 EDSJO</td><td>97</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>37 BAER</td><td>96</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>16 BEREZINSKY</td><td>95</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>38 FALK</td><td>95</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>39 DREES</td><td>93</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>40 FALK</td><td>93</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>39 KELLEY</td><td>93</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>41 MIZUTA</td><td>93</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>42 LOPEZ</td><td>92</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>43 MCDONALD</td><td>92</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>44 GRIEST</td><td>91</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>45 NOJIRI</td><td>91</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>46 OLIVE</td><td>91</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>47 ROSZKOWSKI</td><td>91</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>48 GRIEST</td><td>90</td><td>COSM</td></tr><tr><td>&lt; 600 GeV</td><td>46 OLIVE</td><td>89</td><td>COSM</td></tr><tr><td>none 100 eV - 15 GeV</td><td>SREDNICKI</td><td>88</td><td>COSM</td></tr></tbody></table>
none 100 eV-5 GeV

ELLIS

84 COSM $\tilde{\gamma}$; for $m_{\tilde{\gamma}}=100$ GeV

GOLDBERG

83 COSM $\tilde{\gamma}$

49 KRAUSS

83 COSM $\tilde{\gamma}$

VYSOTSKII

83 COSM $\tilde{\gamma}$

1 ELLIS 00 updates ELLIS 98. Uses LEP $e^+e^-$ data at $\sqrt{s}=202$ and 204 GeV to improve bound on neutralino mass to 51 GeV when scalar mass universality is assumed and 46 GeV when Higgs mass universality is relaxed. Limits on $\tan\beta$ improve to $> 2.7$ ($\mu>0$), $> 2.2$ ($\mu<0$) when scalar mass universality is assumed and $> 1.9$ (both signs of $\mu$) when Higgs mass universality is relaxed.

2 ATHRON 17b places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using all Run I and the 13 fb$^{-1}$ 13 TeV Run II LHC searches and other experimental data.

3 BECHTLE 16 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using all Run I LHC searches.

4 BAGNASCHI 15 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using all Run I LHC searches.

5 Implications of the LHC result on the Higgs mass and on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

6 BUCHMUELLER 14a places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using indirect experimental searches using the 20 fb$^{-1}$ 8 TeV and the 5 fb$^{-1}$ 7 TeV LHC and the LUX data.

7 ROSZKOWSKI 14 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using Bayesian statistics and indirect experimental searches using the 20 fb$^{-1}$ LHC and the LUX data.

8 CABRERA 13 and STREGE 13 place constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry with and without non-universal Higgs masses using the 5.8 fb$^{-1}$, $\sqrt{s}=7$ TeV ATLAS supersymmetry searches and XENON100 results.

9 ELLIS 13b place constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry with and without Higgs mass universality. Models with universality below the GUT scale are also considered.

10 BALAZS 12 and STREGE 12 place constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using the 1 fb$^{-1}$ LHC supersymmetry searches, the 5 fb$^{-1}$ Higgs mass constraints, both with $\sqrt{s}=7$ TeV, and XENON100 results.

11 BECHTLE 12 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using indirect experimental searches, using the 5 fb$^{-1}$ LHC and XENON100 data.

12 BESKIDT 12 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using indirect experimental searches, the 5 fb$^{-1}$ LHC and the XENON100 data.

13 BELANGER 04 and BOTTINO 12 (see also BOTTINO 03, BOTTINO 03A and BOTTINO 04) do not assume gaugino or scalar mass unification.

14 FENG 12b places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry and large fermion masses using the 1 fb$^{-1}$ LHC supersymmetry searches, the 5 fb$^{-1}$ LHC Higgs mass constraints both with $\sqrt{s}=7$ TeV, and XENON100 results.

15 BUCHMUELLER 11 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using indirect experimental searches and including supersymmetry breaking relations between A and B parameters.

16 Places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry but non-Universal Higgs masses.

17 ELLIS 10 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry with universality above the GUT scale.

18 BUCHMUELLER 09 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using indirect experimental searches.

19 DREINER 9 show that in the general MSSM with non-universal gaugino masses there exists no model-independent laboratory bound on the mass of the lightest neutralino. An essentially massless $\chi_1^0$ is allowed by the experimental and observational data, imposing some constraints on other MSSM parameters, including $M_2$, $\mu$ and the slepton and squark masses.

20 BUCHMUELLER 08 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry using indirect experimental searches.

21 CALIBBI 07 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry with universality above the GUT scale including the effects of right-handed neutrinos.

22 ELLIS 07 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry with universality below the GUT scale.

23 ALLANACH 06 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

24 DE-AUSTRI 06 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

25 BALTZ 04 places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

26 Limit assumes a pseudo scalar mass < 200 GeV. For larger pseudo scalar masses, $m_\chi > 18(29)$ GeV for $\tan\beta = 50(10)$. Bounds from WMAP, $(g-2)\mu, b \to s\gamma$, LEP.

27 ELLIS 04b places constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry including supersymmetry breaking relations between A and B parameters. See also ELLIS 03d.

28 PIERCE 04a places constraints on the SUSY parameter space in the framework of models with very heavy scalar masses.

29 BAER 03, CHATTOPADHYAY 03, ELLIS 03c and LAHANAS 03 place constraints on the SUSY parameter space in the framework of $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry based on WMAP results for the cold dark matter density.

30 BOEHM 00b and ELLIS 03 place constraints on the SUSY parameter space in the framework of minimal $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry. Includes the effect of $\chi-\tilde{\chi}$ co-annihilations.

31 LAHANAS 02 places constraints on the SUSY parameter space in the framework of minimal $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry. Focuses on the role of pseudo-scalar Higgs exchange.

32 BARGER 01c use the cosmic relic density inferred from recent CMB measurements to constrain the parameter space in the framework of minimal $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

33 ELLIS 01b places constraints on the SUSY parameter space in the framework of minimal $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry. Focuses on models with large $\tan\beta$.

34 FENG 00 explores cosmologically allowed regions of MSSM parameter space with multi-TeV masses.

35 ELLIS 98b assumes a universal scalar mass and radiative supersymmetry breaking with universal gaugino masses. The upper limit to the LSP mass is increased due to the inclusion of $\chi-\tilde{\chi}_R$ coannihilations.

36 EDSJO 97 included all coannihilation processes between neutralinos and charginos for any neutralino mass and composition.

37 Notes the location of the neutralino Z resonance and h resonance annihilation corridors in minimal supergravity models with radiative electroweak breaking.

38 Mass of the bino (=LSP) is limited to $m_{\tilde{B}} \lesssim 350$ GeV for $m_t = 174$ GeV.

39 DREES 93, KELLEY 93 compute the cosmic relic density of the LSP in the framework of minimal $N=1$ supergravity models with radiative breaking of the electroweak gauge symmetry.

40 FALK 93 relax the upper limit to the LSP mass by considering sfermion mixing in the MSSM.

41 MIZUTA 93 include coannihilations to compute the relic density of Higgsino dark matter.

42 LOPEZ 92 calculate the relic LSP density in a minimal SUSY GUT model.

43 MCDONALD 92 calculate the relic LSP density in the MSSM including exact tree-level annihilation cross sections for all two-body final states.

44 GRIEST 91 improve relic density calculations to account for coannihilations, pole effects, and threshold effects.

45 NOJRI 91 uses minimal supergravity mass relations between squarks and sleptons to narrow cosmologically allowed parameter space.

46 Mass of the bino (=LSP) is limited to $m_{\tilde{B}} \lesssim 350$ GeV for $m_t \le 200$ GeV. Mass of the higgsino (=LSP) is limited to $m_{\tilde{H}} \lesssim 1$ TeV for $m_t \le 200$ GeV.

47 ROSZKOWSKI 91 calculates LSP relic density in mixed gaugino/higgsino region.

48 Mass of the bino (=LSP) is limited to $m_{\tilde{B}} \lesssim 550$ GeV. Mass of the higgsino (=LSP) is limited to $m_{\tilde{H}} \lesssim 3.2$ TeV.

49 KRAUSS 83 finds $m_{\tilde{\gamma}}$ not 30 eV to 2.5 GeV. KRAUSS 83 takes into account the gravitino decay. Find that limits depend strongly on reheated temperature. For example a new allowed region $m_{\tilde{\gamma}}=4-20$ MeV exists if $m_{\text{gravitino}} < 40$ TeV. See figure 2.

Unstable $\tilde{\chi}_1^0$ (Lightest Neutralino) mass limit

Unless otherwise stated, results in this section assume spectra and production rates as evaluated in the MSSM. Unless otherwise stated, the goldstino or gravitino mass $m_{\tilde{G}}$ is assumed to be negligible relative to all other masses. In the following, $\tilde{G}$ is assumed to be undetected and to give rise to a missing energy ($\not{E}$) signature.

Some earlier papers are now obsolete and have been omitted. They were last listed in our PDG 14 edition: K. Olive, et al. (Particle Data Group), Chinese Physics C38 070001 (2014) (http://pdg.lbl.gov).

<table><thead><tr><th>VALUE (GeV)</th><th>CI %</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt; 900</td><td>95</td><td>1 AAD</td><td>23AE ATLS</td><td>2 SFOS &ell;, jets, E<sub>T</sub>, Tn1n1C, m<sub>&chi;<sup>0</sup>1</sub> = 1 GeV</td></tr><tr><td>&gt; 365</td><td>95</td><td>2 AAD</td><td>23AM ATLS</td><td>long-lived &chi;<sup>0</sup><sub>1</sub>, displaced diphoton vertex, Tn1n1A, &tau; = 2 ns</td></tr><tr><td>&gt; 605</td><td>95</td><td>2 AAD</td><td>23AM ATLS</td><td>long-lived &chi;<sup>0</sup><sub>1</sub>, displaced diphoton vertex, Tn1n1B, &tau; = 2 ns</td></tr><tr><td>&gt; 705</td><td>95</td><td>2 AAD</td><td>23AM ATLS</td><td>long-lived &chi;<sup>0</sup><sub>1</sub>, displaced diphoton vertex, Tn1n1C, &tau; = 2 ns</td></tr><tr><td>&gt; 440</td><td>95</td><td>3 AAD</td><td>23CP ATLS</td><td>2 same-sign or 3 &ell;, Tn1n1D, bRPV higgsino decays to &nu;W, &ell;W</td></tr><tr><td>&gt;1180</td><td>95</td><td>4 TUMASYAN</td><td>23AO CMS</td><td>long-lived &chi;<sup>0</sup><sub>1</sub>, &ge; 2 trackless delayed jets + E<sub>T</sub>, Tn1n1B, c&tau; = 0.5 m</td></tr><tr><td>&gt; 990</td><td>95</td><td>4 TUMASYAN</td><td>23AO CMS</td><td>long-lived &chi;<sup>0</sup><sub>1</sub>, &ge; 2 trackless delayed jets + E<sub>T</sub>, Tn1n1B, c&tau; = 3 m</td></tr><tr><td>&gt; 540</td><td>95</td><td>5 AAD</td><td>21Y ATLS</td><td>&ge; 4&ell;, Tch1n12-GGM, &chi;<sup>0</sup><sub>1</sub> &rarr; Z&not;G</td></tr><tr><td>none 7-50</td><td>95</td><td>6 AAIJ</td><td>21V LHCB</td><td>e<sup>&pm;</sup>&mu;<sup>&mpm;</sup>, RPV &chi;<sup>0</sup><sub>1</sub> &rarr; e<sup>&pm;</sup>&mu;<sup>&mpm;</sup>&nu;, 2 ps &lt; &tau; &lt; 50 ps</td></tr><tr><td>&gt;1100</td><td>95</td><td>7 SIRUNYAN</td><td>21AF CMS</td><td>long-lived &chi;<sup>0</sup><sub>1</sub>, RPV &chi;<sup>0</sup><sub>1</sub> &rarr; tbs, &chi;<sup>0</sup><sub>1</sub><sup>223</sup> coupling, 0.6 mm &lt; c&tau; &lt; 70 mm</td></tr><tr><td>&gt; 800</td><td>95</td><td>8 SIRUNYAN</td><td>21M CMS</td><td>&ell;<sup>&pm;</sup>&ell;<sup>&mpm;</sup> + E<sub>T</sub>, Tn1n1C</td></tr><tr><td>&gt; 650</td><td>95</td><td>9 SIRUNYAN</td><td>21M CMS</td><td>&ell;<sup>&pm;</sup>&ell;<sup>&mpm;</sup> + E<sub>T</sub>, Tn1n1B</td></tr><tr><td>&gt; 380</td><td>95</td><td>9 AAD</td><td>20AN ATLS</td><td>2&gamma; + E<sub>T</sub>, Tn1n1A, GMSB</td></tr><tr><td>&gt; 525</td><td>95</td><td>10 SIRUNYAN</td><td>19CA CMS</td><td>&chi;<sup>0</sup><sub>1</sub> &rarr; &gamma;G, GMSB, SPS8, c&tau;=1 m</td></tr><tr><td>&gt; 290</td><td>95</td><td>11 SIRUNYAN</td><td>19CI CMS</td><td>&ge; 1 H(&rarr;&gamma;&gamma;) + jets + E<sub>T</sub>, Tn1n1A, GMSB</td></tr><tr><td>&gt; 230</td><td>95</td><td>11 SIRUNYAN</td><td>19CI CMS</td><td>&ge; 1 H(&rarr;&gamma;&gamma;) + jets + E<sub>T</sub>, Tn1n1B, GMSB</td></tr></tbody></table>
# Searches Particle Listings

## Supersymmetric Particle Searches

<table><tbody><tr><td>&gt; 930</td><td>95</td><td><sup>12</sup>SIRUNYAN</td><td>19K CMS</td><td>γ + lepton + E<sub>T</sub>, Tch1n1A</td></tr><tr><td>none 130–230,<br>290–880</td><td>95</td><td><sup>13</sup>AABOUD</td><td>18CK ATLS</td><td>2H (→ bb) + E<sub>T</sub>, Tn1n1A, GMSB</td></tr><tr><td>&gt; 295</td><td>95</td><td><sup>14</sup>AABOUD</td><td>18Z ATLS</td><td>≥ 4ℓ, GMSB, Tn1n1C</td></tr><tr><td>&gt; 180</td><td>95</td><td><sup>15</sup>SIRUNYAN</td><td>18AO CMS</td><td>ℓ±ℓ± or ≥ 3ℓ, Tn1n1A</td></tr><tr><td>&gt; 260</td><td>95</td><td><sup>15</sup>SIRUNYAN</td><td>18AO CMS</td><td>ℓ±ℓ± or ≥ 3ℓ, Tn1n1B</td></tr><tr><td>&gt; 450</td><td>95</td><td><sup>15</sup>SIRUNYAN</td><td>18AO CMS</td><td>ℓ±ℓ± or ≥ 3ℓ, Tn1n1C</td></tr><tr><td>&gt; 750</td><td>95</td><td><sup>16</sup>SIRUNYAN</td><td>18AP CMS</td><td>Combination of searches, GMSB,<br>Tn1n1A</td></tr><tr><td>&gt; 650</td><td>95</td><td><sup>16</sup>SIRUNYAN</td><td>18AP CMS</td><td>Combination of searches, GMSB,<br>Tn1n1B</td></tr><tr><td>&gt; 690</td><td>95</td><td><sup>16</sup>SIRUNYAN</td><td>18AP CMS</td><td>Combination of searches, GMSB,<br>Tn1n1C</td></tr><tr><td>&gt; 500</td><td>95</td><td><sup>17</sup>SIRUNYAN</td><td>18AR CMS</td><td>ℓ±ℓ<sup>+</sup> + jets + E<sub>T</sub>, GMSB, Tn1n1B</td></tr><tr><td>&gt; 650</td><td>95</td><td><sup>17</sup>SIRUNYAN</td><td>18AR CMS</td><td>ℓ±ℓ<sup>+</sup> + jets + E<sub>T</sub>, GMSB, Tn1n1C</td></tr><tr><td>none 230–770</td><td>95</td><td><sup>18</sup>SIRUNYAN</td><td>18O CMS</td><td>2 H (→ bb) + E<sub>T</sub>, Tn1n1A,<br>GMSB</td></tr><tr><td>&gt; 205</td><td>95</td><td><sup>19</sup>SIRUNYAN</td><td>18X CMS</td><td>≥ 1 H (→ γγ) + jets + E<sub>T</sub>,<br>Tn1n1A, GMSB</td></tr><tr><td>&gt; 130</td><td>95</td><td><sup>19</sup>SIRUNYAN</td><td>18X CMS</td><td>≥ 1 H (→ γγ) + jets + E<sub>T</sub>,<br>Tn1n1B, GMSB</td></tr><tr><td>&gt; 380</td><td>95</td><td><sup>20</sup>KHACHATRY...14L</td><td>14L CMS</td><td>χ̃<sub>1</sub><sup>0</sup> → Z̃G simplified models,<br>GMSB, RPV</td></tr></tbody></table>

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

<table><tbody><tr><td></td><td>21 AAD</td><td>20D</td><td>q̃ → q̃χ̃<sub>1</sub><sup>0</sup>, χ̃<sub>1</sub><sup>0</sup> → ℓℓν, RPV, λ<sub>121</sub> or λ<sub>122</sub> ≠ 0</td></tr><tr><td>none<br>300–1000</td><td>95</td><td>22 AABOUD</td><td>19G ATLS</td><td>χ̃<sub>1</sub><sup>0</sup> → ZG from gluinos as in<br>Tglu1A, GMSB, depending on<br>C<sub>T</sub></td></tr><tr><td></td><td>23 AAIJ</td><td>17Z</td><td>displaced vertex with associated μ</td></tr><tr><td></td><td>24 KHACHATRY...16B X</td><td>CMS</td><td>≥ 3ℓ<sup>+</sup>, RPV, λ or λ' couplings,<br>wino- or higgsino-like neutralinos</td></tr><tr><td></td><td>25 AAD</td><td>14BH ATLS</td><td>2γ + E<sub>T</sub>, GMSB, SPS8</td></tr><tr><td></td><td>26 AAD</td><td>13AP ATLS</td><td>2γ + E<sub>T</sub>, GMSB, SPS8</td></tr><tr><td>none 220–380</td><td>95</td><td>27 AAD</td><td>13Q ATLS</td><td>γ + b + E<sub>T</sub>, higgsino-like neu-<br>tralino, GMSB</td></tr><tr><td></td><td>28 AAD</td><td>13R ATLS</td><td>χ̃<sub>1</sub><sup>0</sup> → μjj, RPV, λ'<sub>211</sub> ≠ 0</td></tr><tr><td></td><td>29 AALTONEN</td><td>13I CDF</td><td>χ̃<sub>1</sub><sup>0</sup> → γ̃G, E<sub>T</sub>, GMSB</td></tr><tr><td>&gt; 220</td><td>95</td><td>30 CHATRCHYAN 13AH CMS</td><td>χ̃<sub>1</sub><sup>0</sup> → γ̃G, GMSB, SPS8, cτ &lt; 500 mm</td></tr><tr><td></td><td>31 AAD</td><td>12CP ATLS</td><td>2γ + E<sub>T</sub>, GMSB</td></tr><tr><td></td><td>32 AAD</td><td>12CT ATLS</td><td>≥ 4ℓ<sup>+</sup>, RPV</td></tr><tr><td></td><td>33 AAD</td><td>12R ATLS</td><td>χ̃<sub>1</sub><sup>0</sup> → μjj, RPV, λ'<sub>211</sub> ≠ 0</td></tr><tr><td></td><td>34 ABAZOV</td><td>12AD D0</td><td>χ̃<sub>1</sub><sup>0</sup> → γ̃Z̃G, GMSB</td></tr><tr><td></td><td>35 CHATRCHYAN 12BK CMS</td><td>12BK CMS</td><td>2γ + E<sub>T</sub>, GMSB</td></tr><tr><td></td><td>36 CHATRCHYAN 11B CMS</td><td>11B CMS</td><td>W̃<sub>0</sub><sup>0</sup> → γ̃G, W̃<sub>0</sub><sup>0</sup> → ℓ±̃G, GMSB</td></tr><tr><td>&gt; 149</td><td>95</td><td>37 AALTONEN</td><td>10 CDF</td><td>p̃p̃ → χ̃x̃, χ̃x̃<sub>2</sub><sup>0</sup> → χ̃<sub>1</sub><sup>±</sup>, χ̃<sub>1</sub><sup>0</sup> → γ̃G, GMSB</td></tr><tr><td>&gt; 175</td><td>95</td><td>38 ABAZOV</td><td>10P D0</td><td>χ̃<sub>1</sub><sup>0</sup> → γ̃G, GMSB</td></tr><tr><td>&gt; 125</td><td>95</td><td>39 ABAZOV</td><td>08F D0</td><td>p̃p̃ → χ̃x̃, χ̃x̃<sub>2</sub><sup>0</sup>, χ̃<sub>1</sub><sup>±</sup>, χ̃<sub>1</sub><sup>0</sup> → γ̃G, GMSB</td></tr><tr><td></td><td>40 ABULENCIA</td><td>07H CDF</td><td>RPV, LL̃E</td></tr><tr><td>&gt; 96.8</td><td>95</td><td>41 ABBIENDI</td><td>06B OPAL</td><td>e<sup>+</sup>e<sup>−</sup> → B̃B̃, (B̃ → G̃γ)</td></tr><tr><td></td><td>42 ABDALLAH</td><td>05B DLPH</td><td>e<sup>+</sup>e<sup>−</sup> → G̃χ̃<sub>1</sub><sup>0</sup>, (χ̃<sub>1</sub><sup>0</sup> → G̃γ)</td></tr><tr><td>&gt; 96</td><td>95</td><td>43 ABDALLAH</td><td>05B DLPH</td><td>e<sup>+</sup>e<sup>−</sup> → G̃χ̃<sub>1</sub><sup>0</sup> → h̃Z̃G̃. Limits are set on m<sub>χ̃<sub>1</sub><sup>0</sup></sub> as a function of its lifetime and of the B(χ̃<sub>1</sub><sup>0</sup> → h̃Z̃G̃) assuming B(χ̃<sub>1</sub><sup>0</sup> → h̃G̃) + B(χ̃<sub>1</sub><sup>0</sup> → Z̃G̃) = 1, see Figure 10.</td></tr></tbody></table>

1. AAD 23A E searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for events with 2 ℓ with same flavour and opposite sign, plus jets and E<sub>T</sub>, defining signal region with the dilepton invariant mass both on- and off-shell with respect to the Z boson. No significant excess above the Standard Model predictions is observed. Limits are set on models of strong and electroweak production. In this case, limits are placed on production of mass-degenerate, higgsino triplet NLSP with χ̃<sub>1</sub><sup>0</sup> → Z̃G in a GGM-like scenario, see Figure 15.

2. AAD 23A M searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for events containing electron/photon pairs with invariant mass compatible with h/Z and originating from a common displaced vertex. No significant excess above the Standard Model predictions is observed. Limits are set on a model where members of a nearly degenerate higgsino triplet are pair-produced, yielding long-lived χ̃<sub>1</sub><sup>0</sup> followed by χ̃<sub>1</sub><sup>0</sup> → h/Z̃G. Limits are set on m<sub>χ̃<sub>1</sub><sup>0</sup></sub> as a function of its lifetime and of the B(χ̃<sub>1</sub><sup>0</sup> → h̃Z̃G̃) assuming B(χ̃<sub>1</sub><sup>0</sup> → h̃G̃) + B(χ̃<sub>1</sub><sup>0</sup> → Z̃G̃) = 1, see Figure 10.

3. AAD 23C P searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for events with 2 ℓ with same charge or 3 ℓ plus at least one jet and E<sub>T</sub>, defining signal region based on 'transverse mass' of the dilepton system, E<sub>T</sub> significance and effective mass. No significant excess above the Standard Model predictions is observed. Limits are set on the mass of a mass-degenerate higgsino triplet decaying into a lepton (neutral or charged) and a W via a bilinear RPV coupling, see figure 14.

4. TUMASYAN 23A O searched in 138 fb⁻¹ of pp collisions at √s = 13 TeV for evidence of neutralino-chargino production in events with nearly trackless and out-of-time jets that are used to identify decays of long-lived particles. No significant excess above the Standard Model expectations is observed. Limits are set on the mass of the long-lived χ̃<sub>1</sub><sup>0</sup> in the model Tn1n1B, see their figures 8-10.

5. AAD 21Y searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for supersymmetry in events with four or more leptons (electrons, muons and tau-leptons). No significant excess above the Standard Model expectations is observed. Limits are set on Tch1n12-GGM, and RPV models similar to Tch1n21, Tglu1A (with q = u, d, s, c, b, with equal branching fractions), and ℓ̃L/ν → ℓ̃ν/χ̃<sub>1</sub><sup>0</sup> (mass-degenerate ℓ̃L and ν̃ of all 3 generations), all with χ̃<sub>1</sub><sup>0</sup> → ℓ±ℓ<sup>+</sup>ν via λ<sub>12k</sub> or λ<sub>133</sub> (where i,k ∈ 1,2), see their Figure 11.

6. AAIJ 21V searched in 5.38 fb⁻¹ of pp collisions at √s = 13 TeV for long-lived particles (LLP) decaying to e±μ∓ν. The LLP can be a χ̃<sub>1</sub><sup>0</sup> in RPV SUSY, or a right-handed neutrino, and can be produced in pairs, in the decay of the Higgs boson, or from charged

current processes. No significant excess above the Standard Model expectations is observed. Limits are set on the cross section times branching ratio for all three production mechanisms, see their Figures 6-8.

7. SIRUNYAN 21A F searched in 140 fb⁻¹ of pp collisions at √s = 13 TeV for supersymmetry in events with two displaced vertices from long-lived particles decaying into multijet or dijet final states. No significant excess above the Standard Model expectations is observed. Limits are set on the gluino mass in the simplified model Tglu2RPV with χ̃<sub>1</sub><sup>0</sup><sub>323</sub> coupling, on the χ̃<sub>1</sub><sup>0</sup> mass in an RPV model with χ̃<sub>1</sub><sup>0</sup> pair production and the RPV decay χ̃<sub>1</sub><sup>0</sup> → tbs with λ''<sub>323</sub> coupling and on the ℓ̃ mass in an RPV model with top squark pair production and the RPV decay ℓ̃ → d̃j̃d̃ with λ''<sub>3ij</sub> coupling, see their Figure 7.

8. SIRUNYAN 21M searched in 137 fb⁻¹ of pp collisions at √s = 13 TeV for supersymmetry in events with two opposite-sign same-flavor leptons (electrons, muons and E<sub>T</sub>). No significant excess above the Standard Model expectations is observed. Limits are set on the gluino mass in the simplified model Tglu4C, see their Figure 10, on the χ̃<sub>2</sub><sup>0</sup> and χ̃<sub>1</sub><sup>±</sup> mass in Tch1n2Fa, see their Figure 11, on the χ̃<sub>1</sub><sup>0</sup> mass in Tn1n1C and Tn1n1B for m<sub>χ̃<sub>2</sub><sup>0</sup></sub>=m<sub>χ̃<sub>1</sub><sup>0</sup></sub>=m<sub>χ̃<sub>1</sub><sup>0</sup></sub>, see their Figure 12. Limits are also set on the light squark mass for the simplified model Tsqk2A, on the sbottom mass in Tsbot3, see their Figure 13, and on the slepton mass in direct electroweak pair production of mass-degenerate left- and right-handed sleptons (electrons and muons), see their Figure 14.

9. AAD 20A N searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for events with two photons and missing transverse momentum. Events are further categorised in terms of lepton or jet multiplicity. No significant excess over the expected background is observed. Limits at 95% C.L. are set on the Higgsino mass in the Tn1n1A simplified model, see their Figure 11.

10. SIRUNYAN 19CA searched in 77.4 fb⁻¹ of pp collisions at √s = 13 TeV for events containing delayed photons in both single and diphoton plus E<sub>T</sub> final states. No excess is observed above the background expected from Standard Model processes. The results are used to set 95% C.L. exclusion limits in the context of GMSB, using the SPS8 benchmark model. For neutralino proper decay lengths of 0.1, 1, 10, and 100 m, masses up to about 320, 525, 360, and 215 GeV are excluded, respectively. See their Fig. 5. The searches involve the simplified models Tglu1D, Tglu4A,B,C, Tsqk4A,4B.

11. SIRUNYAN 19CI searched in 77.5 fb⁻¹ of pp collisions at √s = 13 TeV for events with one or more high-momentum Higgs bosons, decaying to pairs of photons, jets and E<sub>T</sub>. No significant excess above the Standard Model expectations is observed. Limits are set on the bottom mass in the Tsbot4 simplified model, see Figure 3, and on the wino mass in the Tch1n2E simplified model, see their Figure 4. Limits are also set on the higgsino mass in the Tn1n1A and Tn1n1B simplified models, see their Figure 5.

12. SIRUNYAN 19K searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for events with a photon, an electron or muon, and large E<sub>T</sub>. No significant excess above the Standard Model expectations is observed. In the framework of GMSB, limits are set on the chargino and neutralino mass in the Tch1n1A simplified model, see their Figure 6. Limits are also set on the gluino mass in the Tglu4A simplified model, and on the squark mass in the Tsqk4A simplified model, see their Figure 7.

13. AABOUD 18CK searched for events with at least 3 b-jets and large missing transverse energy in two datasets of pp collisions at √s = 13 TeV of 36.1 fb⁻¹ and 24.3 fb⁻¹ depending on the trigger requirements. The analyses aimed to reconstruct two Higgs bosons decaying to pairs of b-quarks. No significant excess above the Standard Model expectations is observed. Limits are set on the higgsino mass in the Tn1n1A simplified model, see their Figure 15(a). Constraints are also presented as a function of the BR of Higgsino decaying into an higgs boson and a gravitino, see their Figure 15(b).

14. AABOUD 18Z searched in 36.1 fb⁻¹ of pp collisions at √s = 13 TeV for events containing four or more charged leptons (electrons, muons and up to two hadronically decaying taus). No significant deviation from the expected SM background is observed. Limits are set on the Higgsino mass in simplified models of general gauge mediated supersymmetry Tn1n1A/Tn1n1B/Tn1n1C, see their Figure 9. Limits are also set on the wino, slepton, sneutrino and gluino mass in a simplified model of NLSP pair production with R-parity violating decays of the LSP via λ<sub>12k</sub> or λ<sub>133</sub> to charged leptons, see their Figures 7, 8.

15. SIRUNYAN 18A O searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for direct electroweak production of charginos and neutralinos in events with either two or more leptons (electrons or muons) of the same electric charge, or with three or more leptons, which can include up to two hadronically decaying tau leptons. No significant excess above the Standard Model expectations is observed. Limits are set on the chargino/neutralino mass in the Tch1n2A, Tch1n2H, Tch1n2D, Tch1n2E and Tch1n2F simplified models, see their Figures 14, 15, 16, 17 and 18. Limits are also set on the higgsino mass in the Tn1n1A, Tn1n1B and Tn1n1C simplified models, see their Figure 19.

16. SIRUNYAN 18AP searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for direct electroweak production of charginos and neutralinos by combining a number of previous and new searches. No significant excess above the Standard Model expectations is observed. Limits are set on the chargino/neutralino mass in the Tch1n2E, Tch1n2F and Tch1n2L simplified models, see their Figures 7, 8, 9 and 10. Limits are also set on the higgsino mass in the Tn1n1A, Tn1n1B and Tn1n1C simplified models, see their Figure 11, 12, 13 and 14.

17. SIRUNYAN 18AR searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for events containing two opposite-sign leptons (electrons or muons), jets and E<sub>T</sub>. No significant excess above the Standard Model expectations is observed. Limits are set on the gluino mass in the Tglu4C simplified model, see their Figure 7. Limits are also set on the chargino in the Tglu4C simplified model, see their Figure 8, and on the higgsino mass in the Tn1n1B and Tn1n1C simplified models, see their Figure 9. Finally, limits are set on the sbottom mass in the Tsbot3 simplified model, see their Figure 10.

18. SIRUNYAN 18O searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for events with two Higgs bosons, decaying to pairs of b-quarks, and large E<sub>T</sub>. No significant excess above the Standard Model expectations is observed. Limits are set on the Higgsino mass in the Tn1n1A simplified model, see their Figure 9.

19. SIRUNYAN 18X searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for events with one or more high-momentum Higgs bosons, decaying to pairs of photons, jets and E<sub>T</sub>. The razor variables (MR and R²) are used to categorise the events. No significant excess above the Standard Model expectations is observed. Limits are set on the sbottom mass in the Tsbot4 simplified model and on the wino mass in the Tch1n2E simplified model, see their Figure 5. Limits are also set on the higgsino mass in the Tn1n1A and Tn1n1B simplified models, see their Figure 6.

20. KHACHATRYAN 14L searched in 19.5 fb⁻¹ of pp collisions at √s = 8 TeV for evidence of direct pair production of neutralinos with Higgs or Z-bosons in the decay chain, leading to HH, HZ and ZZ final states with missing transverse energy. The decays of 16-20.
a Higgs boson to a b-quark pair, to a photon pair, and to final states with leptons are considered in conjunction with hadronic and leptonic decay modes of the Z and W bosons. No significant excesses over the expected SM backgrounds are observed. The results are interpreted in the context of GMSB simplified models where the decays $\tilde{\chi}_1^0 \to H\bar{G}$ or $\tilde{\chi}_1^0 \to Z\bar{G}$ take place either 100% or 50% of the time, see Figs. 16–20.

21 AAD 20D searched in 32.8 fb⁻¹ of pp collisions at $\sqrt{s} = 13$ TeV for events containing an oppositely charge lepton pair (e, eµ or eµ) coming from long-lived neutralinos decaying through the R-parity-violating decay $\tilde{\chi}_1^0 \to \ell\ell\nu$ with $\lambda_{121} \neq 0$ or $\lambda_{122} \neq 0$. No excess over the expected background is observed. Limits are derived for decay lengths of the neutralino between 1 mm and 10 m in a scenario where a squark-antisquark pair is produced, with the squark decaying to a quark and a $\tilde{\chi}_1^0$, with either $\tilde{\chi}_1^0 \to e\nu e\mu\nu$ ($\lambda_{121} \neq 0$) or $\tilde{\chi}_1^0 \to e\mu\nu/\mu\mu\nu$ ($\lambda_{122} \neq 0$), see their Figures 4 and 5.

22 AABOUD 19G searched in 32.9 fb⁻¹ of pp collisions at $\sqrt{s} = 13$ TeV for evidence of neutralinos decaying into a Z-boson and a gravitino, in events characterized by the presence of dimuon vertices with displacements from the pp interaction point in the range of 1400 cm. Neutralinos are assumed to be produced in the decay chain of gluinos as in Tglu1A models. No significant excess is observed in the number of vertices relative to the predicted background. In GGM with a gluino mass of 1100 GeV, neutralino masses in the range 300–1000 GeV are excluded for certain values of $\tau_c$, see their Figure 7.

23 AA1J 17Z searched in 1 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV and in 2 fb⁻¹ of pp collisions at $\sqrt{s} = 8$ TeV for events containing a displaced vertex with one associated high transverse momentum $\mu$. No excess is observed above the background expected from Standard Model processes. The results are used to set 95% C.L. exclusion limits in the contact of gauge-mediated supersymmetric breaking models, with the lightest neutralino being the next-to-lightest supersymmetric particle and decaying with a lifetime in the range from 0.25 ns to about 100 ns into a photon and a gravitino. For limits on the NLSP lifetime versus $\Lambda$ plane, for the SPS8 model, see their Fig. 5 and Fig. 6.

24 KHACHATRYAN 16X8 searched in 19.5 fb⁻¹ of pp collisions at $\sqrt{s} = 8$ TeV for events containing 3 or more leptons coming from the electroweak production of wino- or higgsino-like neutralinos, assuming non-zero R-parity-violating leptonic couplings $\lambda_{122}$, $\lambda_{123}$, and $\lambda_{233}$ or semileptonic couplings $\lambda'_{131}$, $\lambda'_{233}$, $\lambda'_{131}$, and $\lambda'_{233}$. No excess over the expected background is observed and limits are derived on the neutralino mass, see Figs. 24 and 25.

25 AAD 14BH searched in 20.3 fb⁻¹ of pp collisions at $\sqrt{s} = 8$ TeV for events containing non-pointing photons in a diphoton plus missing transverse energy final state. No excess is observed above the background expected from Standard Model processes. The results are used to set 95% C.L. exclusion limits in the contact of gauge-mediated supersymmetric breaking models, with the lightest neutralino being the next-to-lightest supersymmetric particle and decaying with a lifetime in the range from 0.25 ns to about 100 ns into a photon and a gravitino. For limits on the NLSP lifetime versus $\Lambda$ plane, for the SPS8 model, see their Fig. 7.

26 AAD 13AP searched in 4.8 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events containing non-pointing photons in a diphoton plus missing transverse energy final state. No excess is observed above the background expected from Standard Model processes. The results are used to set 95% C.L. exclusion limits in the contact of gauge-mediated supersymmetric breaking models, with the lightest neutralino being the next-to-lightest supersymmetric particle and decaying with a lifetime in excess of 0.25 ns into a photon and a gravitino. For limits in the NLSP lifetime versus $\Lambda$ plane, for the SPS8 model, see their Fig. 8.

27 AAD 13Q searched in 4.7 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events containing a high-$p_T$ isolated photon, at least one jet identified as originating from a bottom quark, and high missing transverse momentum. Such signatures may originate from supersymmetric models with gauge-mediated supersymmetry breaking in events in which one of a pair of higgsino-like neutralinos decays into a photon and a gravitino while the other decays into a Higgs boson and a gravitino. No significant excess above the expected background was found and limits were set on the neutralino mass in a generalized GMSB model (GGM) with a higgsino-like neutralino NLSP, see their Fig. 4. Intermediate neutralino masses between 220 and 380 GeV are excluded at 95% C.L., regardless of the squark and gluino masses, purely on the basis of the expected weak production.

28 AAD 13R looked in 4.4 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events containing new, heavy particles that decay at a significant distance from their production point into a final state containing a high-momentum muon and charged hadrons. No excess over the expected background is observed and limits are placed on the production cross-section of neutralinos via squarks for various $m_{\tilde{q}}$, $m_{\tilde{\chi}_1^0}$ in an R-parity violating scenario with $\lambda'_{211} \neq 0$, as a function of the neutralino lifetime, see their Fig. 6.

29 AALTONEN 13I searched in 6.3 fb⁻¹ of $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV for events containing $E_T$ and a delayed photon that arrives late in the detector relative to the time expected from prompt production. No evidence of delayed photon production is observed.

30 CHATRYAN 13AH searched in 4.9 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events containing $E_T$ and a delayed photon that arrives late in the detector relative to the time expected from prompt production. No significant excess above the expected background was found and limits were set on the pair production of $\tilde{\chi}_1^0$ depending on the neutralino proper decay length, see Fig. 8.

31 AAD 12CP searched in 4.8 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events with two photons and $E_T$ due to $\tilde{\chi}_1^0 \to \gamma\bar{G}$ decays in a GMSB framework. No significant excess above the expected background was found and limits were set on the neutralino mass in a generalized GMSB model (GGM) with a bino-like neutralino NLSP, see Figs. 6 and 7. The other sparticle masses were decoupled, $\tan\beta = 2$ and $c\tau_N L_{\text{SP8}} < 0.1$ mm. Also, in the framework of the SPS8 model, limits are presented in Fig. 8.

32 AAD 12CT searched in 4.7 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events containing four or more leptons (electrons or muons) and either moderate values of missing transverse momentum or large effective mass. No significant excess is found in the data. Limits are presented in a simplified model of R-parity violating supersymmetry in which charginos are pair-produced and then decay into a W-boson and a $\tilde{\chi}_1^0$, which in turn decays through an RPV coupling into two charged leptons ($e^+e^-$ or $\mu^+\mu^+$) and a neutrino. In this model, limits are set on the neutralino mass as a function of the chargino mass, see Fig. 3a. Limits are also set in an R-parity violating mSUGRA model, see Fig. 3b.

33 AAD 12R looked in 33 pb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events containing new, heavy particles that decay at a significant distance from their production point into a final state containing a high-momentum muon and charged hadrons. No excess over the expected background is observed and limits are placed on the production cross-section of neutralinos via squarks for various ($m_{\tilde{q}}, m_{\tilde{\chi}_1^0}$) in an R-parity violating scenario with $\lambda'_{211} \neq 0$, as a function of the neutralino lifetime, see their Fig. 8. Superseded by AAD 13R.

34 ABAZOV 12AD looked in 6.2 fb⁻¹ of pp collisions at $\sqrt{s} = 1.96$ TeV for events with a photon, a Z-boson, and large $E_T$ in the final state. This topology corresponds to a GMSB model where pairs of neutralino NLSPs are either pair produced promptly or from decays of other supersymmetric particles and then decay to either $Z\bar{G}$ or $\gamma\bar{G}$. No significant excess over the SM expectation is observed and a limit at 95% C.L. on the cross section is derived as a function of the effective SUSY breaking scale $\Lambda$, see Fig. 3. Assuming $N_{mes} = 2$, $M_{mes} = 3$, $\tan\beta = 3$, $\mu = 0.75 M_1$, and $C_{grav} = 1$, the model is excluded at 95% C.L. for values of $\Lambda < 87$ TeV.

35 CHATRYCHAN 12BK searched in 2.23 fb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events with two photons and large $E_T$ due to $\tilde{\chi}_1^0 \to \gamma\bar{G}$ decays in a GMSB framework. No significant excess above the expected background was found and limits were set on the pair production of $\tilde{\chi}_1^0$ depending on the neutralino lifetime, see Fig. 6.

36 CHATRYCHAN 11B looked in 35 pb⁻¹ of pp collisions at $\sqrt{s} = 7$ TeV for events with an isolated lepton (e or $\mu$), a photon and $E_T$ which may arise in a generalized gauge mediated model from the decay of Wino-like NLSPs. No evidence for an excess over the expected background is observed. Limits are derived in the plane of squark/gluino mass versus Wino mass (see Fig. 4). Mass degeneracy of the produced squarks and gluinos is assumed.

37 AALTONEN 10 searched in 2.6 fb⁻¹ of $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV for diphoton events with large $E_T$. They may originate from the production of $\tilde{\chi}^\pm$ in pairs or associated to a $\tilde{\chi}_1^0$, decaying into $\tilde{\chi}_1^0$ which itself decays in GMSB to $\gamma\bar{G}$. There is no excess of events beyond expectation. An upper limit on the cross section is calculated in the GMSB model as a function of the $\tilde{\chi}_1^0$ mass and lifetime, see their Fig. 2. A limit is derived on the $\tilde{\chi}_1^0$ mass of 149 GeV for $\tau_{\tilde{\chi}_1^0} \ll 1$ ns, which improves the results of previous searches.

38 ABAZOV 10P looked in 6.3 fb⁻¹ of $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV for events with at least two isolated $\gamma$s and large $E_T$. These could be the signature of $\tilde{\chi}_2^0$ and $\tilde{\chi}_1^\pm$ production, decaying to $\tilde{\chi}_1^0$ and finally $\tilde{\chi}_1^0 \to \gamma\bar{G}$ in a GMSB framework. No significant excess over the SM expectation is observed, and a limit at 95% C.L. on the cross section is derived for $N_{mes} = 1$, $\tan\beta = 15$ and $\mu > 0$, see their Fig. 2. This allows them to set a limit on the effective SUSY breaking scale $\Lambda > 124$ TeV, from which the excluded $\tilde{\chi}_1^0$ mass range is obtained.

39 ABAZOV 08F looked in 1.1 fb⁻¹ of $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV for diphoton events with large $E_T$. They may originate from the production of $\tilde{\chi}^\pm$ in pairs or associated to a $\tilde{\chi}_2^0$, decaying to a $\tilde{\chi}_1^0$ which itself decays promptly in GMSB to $\tilde{\chi}_1^0 \to \gamma\bar{G}$. No significant excess was found compared to the background expectation. A limit is derived on the masses of SUSY particles in the GMSB framework for $M = 2\Lambda$, $N = 1$, $\tan\beta = 15$ and $\mu > 0$, see Figure 2. It also excludes $\Lambda < 91.5$ TeV. The superseded results of ABAZOV 05A. Superseded by ABAZOV 10P.

40 ABULENCIA 07H searched in 346 pb⁻¹ of $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV for events with at least three leptons (e or $\mu$) from the decay of $\tilde{\chi}_1^0$ via $L\bar{L}$ couplings. The results are consistent with the hypothesis of no signal. Upper limits on the cross-section are extracted and a limit is derived in the framework of mSUGRA on the masses of $\tilde{\chi}_1^0$ and $\tilde{\chi}_1^0$, see e.g. their Fig. 3 and Tab. II.

41 ABBIENDI 06B used 600 pb⁻¹ of data from $\sqrt{s} = 189-209$ GeV. They look for events with diphons + $E_T$ final states originating from prompt decays of pair-produced neutralinos in a GMSB scenario with $\tilde{\chi}_1^0$ NLSP. Limits on the cross-section are computed as a function of $m(\tilde{\chi}_1^0)$, see their Fig. 14. The limit on the $\tilde{\chi}_1^0$ mass is for a pure Bino state assuming a prompt decay, with lifetimes up to $10^{-9}$s. Supersedes the results of ABBIENDI 04N.

42 ABALLALLAH 05B use data from $\sqrt{s} = 180-209$ GeV. They look for events with single photons + $E_T$ final states. Limits are computed in the plane ($m(\tilde{G}), m(\tilde{\chi}_1^0)$), shown in their Fig. 9b for a pure Bino state in the GMSB framework and in Fig. 9c for a no-scale supergravity model. Supersedes the results of ABREU 00Z.

43 ABALLALLAH 05B use data from $\sqrt{s} = 130-209$ GeV. They look for events with diphons + $E_T$ final states and single photons not pointing to the vertex, expected in GMSB when the $\tilde{\chi}_1^0$ is the NLSP. Limits are computed in the plane ($m(\tilde{G}), m(\tilde{\chi}_1^0)$), see their Fig. 10. The lower limit is derived on the $\tilde{\chi}_1^0$ mass for a pure Bino state assuming a prompt decay and $m_{\tilde{e}_R} = m_{\tilde{e}_L} = 2 m_{\tilde{\chi}_1^0}$. It improves to 100 GeV for $m_{\tilde{e}_R} = m_{\tilde{e}_L} = 1.1 m_{\tilde{\chi}_1^0}$, and the limit in the plane ($m(\tilde{\chi}_1^0), m(\tilde{e}_R)$) is shown in Fig. 10b. For long-lived neutralinos, cross-section limits are displayed in their Fig. 11. Supersedes the results of ABREU 00Z.

$\tilde{\chi}_2^0$, $\tilde{\chi}_3^0$, $\tilde{\chi}_4^0$ (Neutralinos) mass limits

Neutralinos are unknown mixtures of photinos, z-inos, and neutral higgsinos (the supersymmetric partners of photons and of Z and Higgs bosons). The limits here apply only to $\tilde{\chi}_1^0$, $\tilde{\chi}_2^0$, and $\tilde{\chi}_4^0$. $\tilde{\chi}_1^0$ is the lightest supersymmetric particle (LSP); see $\tilde{\chi}_1^0$ Mass Limits. It is not possible to quote rigorous mass limits because they are extremely model dependent; i.e. they depend on branching ratios of various $\tilde{\chi}_1^0$ decay modes, on the masses of decay products ($\tilde{e}, \tilde{\gamma}, \tilde{q}, \tilde{g}$), and on the $\tilde{e}$ mass exchanged in $e^+e^- \to \tilde{\chi}_1^0 \tilde{\chi}_1^0$. Limits arise either from direct searches, or from the MSSM constraints set on the gaugino and higgsino mass parameters $M_2$ and $\mu$ through searches for lighter charginos and neutralinos. Often limits are given as contour plots on the $m_{\tilde{\chi}_1^0} - m_{\tilde{e}}$ plane vs other parameters. When specific assumptions are made, e.g. the neutralino is a pure photino ($\tilde{\gamma}$), pure z-ino ($\tilde{Z}$), or pure neutral higgsino ($\tilde{H}^0$), the neutralinos will be labelled as such.

Limits obtained from $e^+e^-$ collisions at energies up to 136 GeV, as well as other limits from different techniques, are now superseded and have not been included in this compilation. They can be found in the 1998 Edition (The European Physical Journal C31 (1998)) of this Review. Some later papers (The now obsolete and have been omitted). They were last listed in our PDG 14 edition: K. Olive, et al. (Particle Data Group), Chinese Physics C38 070001 (2014) (http://pdg.bnl.gov).

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt; 820</td><td>95</td><td>1 AAD</td><td>23AE ATLS</td><td>2 SFOS &ell;, jets, E<sub>T</sub>, Tchiln2Fa, m<sub>&chi;<sub>1</sub><sup>0</sup></sub> = 1 GeV</td></tr><tr><td>none 260-420</td><td>95</td><td>2 AAD</td><td>23CI ATLS</td><td>1 &ell; + jets + E<sub>T</sub>, Tchiln2J, m<sub>&chi;<sub>1</sub><sup>0</sup></sub> = 0 GeV</td></tr></tbody></table>
# Searches Particle Listings

## Supersymmetric Particle Searches

<table>
  <tbody>
    <tr>
      <td>&gt; 230</td>
      <td>95</td>
      <td>3 AAD</td>
      <td>23CI ATLS</td>
      <td>1ℓ + jets + E<sub>T</sub>, Tchi1n2E, m<sub>χ̃<sub>2</sub></sub> - m<sub>χ̃<sub>1</sub></sub> = 133 GeV</td>
    </tr>
    <tr>
      <td>&gt; 450</td>
      <td>95</td>
      <td>3 AAD</td>
      <td>23CI ATLS</td>
      <td>1ℓ + jets + E<sub>T</sub>, Tchi1n2E, m<sub>χ̃<sub>2</sub></sub> - m<sub>χ̃<sub>1</sub></sub> = 260 GeV</td>
    </tr>
    <tr>
      <td>&gt; 525</td>
      <td>95</td>
      <td>4 AAD</td>
      <td>23CP ATLS</td>
      <td>2 same-sign ℓ, Tchi1n2E, winobino, m<sub>χ̃<sub>1</sub></sub> = 1 GeV</td>
    </tr>
    <tr>
      <td>none 200-250</td>
      <td>95</td>
      <td>4 AAD</td>
      <td>23CP ATLS</td>
      <td>2 same-sign ℓ, Tchi1n2F, winobino, m<sub>χ̃<sub>1</sub></sub> = 1 GeV</td>
    </tr>
    <tr>
      <td>none 200-585</td>
      <td>95</td>
      <td>5 AAD</td>
      <td>23CR ATLS</td>
      <td>RPV, 2 same-sign, 3, 4 ℓ, 1, 2 b-jets, higgsino production with χ̃ → b + ℓ/ν + t/b via χ̃<sub>133</sub> coupling</td>
    </tr>
    <tr>
      <td>none 200-670</td>
      <td>95</td>
      <td>5 AAD</td>
      <td>23CR ATLS</td>
      <td>RPV, 2 same-sign, 3, 4 ℓ, 1, 2 b-jets, wino production with χ̃ → b + ℓ/ν + t/b via χ̃<sub>133</sub> coupling</td>
    </tr>
    <tr>
      <td>&gt;1050</td>
      <td>95</td>
      <td>6 HAYRAPETY...23E</td>
      <td>CMS</td>
      <td>γ + jets + E<sub>T</sub>, Tchi1chi1A</td>
    </tr>
    <tr>
      <td>&gt; 450</td>
      <td>95</td>
      <td>6 HAYRAPETY...23E</td>
      <td>CMS</td>
      <td>γ + jets + E<sub>T</sub>, Tn1n2A</td>
    </tr>
    <tr>
      <td>none 290-670</td>
      <td>95</td>
      <td>7 TUMASYAN</td>
      <td>23B CMS</td>
      <td>2 AK8 jets + 2-6 AK4 jets + E<sub>T</sub>, Tchi1chi1, m<sub>χ̃<sub>1</sub></sub> = 1 GeV</td>
    </tr>
    <tr>
      <td>none 230-760</td>
      <td>95</td>
      <td>7 TUMASYAN</td>
      <td>23B CMS</td>
      <td>2 AK8 jets + 2-6 AK4 jets + E<sub>T</sub>, Tchi1n2Fb, m<sub>χ̃<sub>1</sub></sub> = 1 GeV</td>
    </tr>
    <tr>
      <td>none 240-970</td>
      <td>95</td>
      <td>7 TUMASYAN</td>
      <td>23B CMS</td>
      <td>2 AK8 jets + 2-6 AK4 jets + E<sub>T</sub>, Tchi1n2Fc, m<sub>χ̃<sub>1</sub></sub> = 1 GeV</td>
    </tr>
    <tr>
      <td>none 300-650</td>
      <td>95</td>
      <td>7 TUMASYAN</td>
      <td>23B CMS</td>
      <td>2 AK8 jets + 2-6 AK4 jets + E<sub>T</sub>, Tn1hBinoA, m<sub>χ̃<sub>1</sub></sub> = 1 GeV</td>
    </tr>
    <tr>
      <td>&gt; 275</td>
      <td>95</td>
      <td>8 TUMASYAN</td>
      <td>22Q CMS</td>
      <td>2 or 3 ℓ (soft), E<sub>T</sub>; Tchi1n2F, wino-bino, m<sub>χ̃<sub>2</sub></sub> - m<sub>χ̃<sub>1</sub></sub> = 10 GeV</td>
    </tr>
    <tr>
      <td>&gt; 205</td>
      <td>95</td>
      <td>8 TUMASYAN</td>
      <td>22Q CMS</td>
      <td>2 or 3 ℓ (soft), E<sub>T</sub>; higgsino model with χ̃<sub>2</sub><sup>0</sup> χ̃<sub>1</sub><sup>±</sup> and χ̃<sub>2</sub><sup>0</sup> χ̃<sub>1</sub><sup>0</sup> prod., m<sub>χ̃<sub>2</sub></sub> - m<sub>χ̃<sub>1</sub></sub> = 7.5 GeV</td>
    </tr>
    <tr>
      <td>&gt; 150</td>
      <td>95</td>
      <td>8 TUMASYAN</td>
      <td>22Q CMS</td>
      <td>2 or 3 ℓ (soft), E<sub>T</sub>; higgsino model with χ̃<sub>2</sub><sup>0</sup> χ̃<sub>1</sub><sup>±</sup> and χ̃<sub>2</sub><sup>0</sup> χ̃<sub>1</sub><sup>0</sup> prod., m<sub>χ̃<sub>2</sub></sub> - m<sub>χ̃<sub>1</sub></sub> = 3 GeV</td>
    </tr>
    <tr>
      <td>&gt;1450</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (flavor-democratic), m<sub>χ̃</sub> = 1/2(m<sub>χ̃<sub>1</sub></sub><sup>±</sup> + m<sub>χ̃<sub>1</sub></sub><sup>0</sup>), m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 850 GeV</td>
    </tr>
    <tr>
      <td>&gt;1360</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (flavor-democratic), m<sub>χ̃</sub> = 1/2(m<sub>χ̃<sub>1</sub></sub><sup>±</sup> + m<sub>χ̃<sub>1</sub></sub><sup>0</sup>), m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt;1290</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (flavor-democratic), m<sub>χ̃</sub> = 0.05m<sub>χ̃<sub>1</sub></sub><sup>±</sup> +0.95m<sub>χ̃<sub>1</sub></sub><sup>0</sup>, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt;1440</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (flavor-democratic), m<sub>χ̃</sub> = 0.95m<sub>χ̃<sub>1</sub></sub><sup>±</sup> +0.05m<sub>χ̃<sub>1</sub></sub><sup>0</sup>, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt;1140</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (lepton in χ̃<sub>1</sub><sup>±</sup> decay is τ), m<sub>χ̃</sub> = 1/2(m<sub>χ̃<sub>1</sub></sub><sup>±</sup> + m<sub>χ̃<sub>1</sub></sub><sup>0</sup>), m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt;1110</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (lepton in χ̃<sub>1</sub><sup>±</sup> decay is τ), m<sub>χ̃</sub> = 0.05m<sub>χ̃<sub>1</sub></sub><sup>±</sup> +0.95m<sub>χ̃<sub>1</sub></sub><sup>0</sup>, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt;1140</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (lepton in χ̃<sub>1</sub><sup>±</sup> decay is τ), m<sub>χ̃</sub> = 0.95m<sub>χ̃<sub>1</sub></sub><sup>±</sup> +0.05m<sub>χ̃<sub>1</sub></sub><sup>0</sup>, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 980</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (leptons in χ̃<sub>1</sub><sup>±</sup> and χ̃<sub>2</sub><sup>0</sup> decays are τ), m<sub>χ̃</sub> = 1/2(m<sub>χ̃<sub>1</sub></sub><sup>±</sup> + m<sub>χ̃<sub>1</sub></sub><sup>0</sup>), m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 905</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (leptons in χ̃<sub>1</sub><sup>±</sup> and χ̃<sub>2</sub><sup>0</sup> decays are τ), m<sub>χ̃</sub> = 0.05m<sub>χ̃<sub>1</sub></sub><sup>±</sup> +0.95m<sub>χ̃<sub>1</sub></sub><sup>0</sup>, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 875</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>same-sign e or μ, 3 or 4 leptons, Tchi1n2B (leptons in χ̃<sub>1</sub><sup>±</sup> and χ̃<sub>2</sub><sup>0</sup> decays are τ), m<sub>χ̃</sub> = 0.95m<sub>χ̃<sub>1</sub></sub><sup>±</sup> +0.05m<sub>χ̃<sub>1</sub></sub><sup>0</sup>, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
  </tbody>
</table>

<table>
  <tbody>
    <tr>
      <td>&gt; 650</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>2 same-sign e or μ, 3 or 4 leptons, Tchi1n2F, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 260</td>
      <td>95</td>
      <td>9 TUMASYAN</td>
      <td>22S CMS</td>
      <td>2 same-sign e or μ, 3 or 4 leptons, Tchi1n2E, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>none 265-305</td>
      <td>95</td>
      <td>10 TUMASYAN</td>
      <td>22V CMS</td>
      <td>3, 4 b-tagged or 2 large-radius jets, E<sub>T</sub>; higgsino χ̃<sub>2</sub><sup>0</sup> χ̃<sub>3</sub><sup>0</sup> prod. with χ̃<sub>2,3</sub> → Hχ̃<sub>1</sub><sup>0</sup>; m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 1 GeV</td>
    </tr>
    <tr>
      <td>&gt; 640</td>
      <td>95</td>
      <td>11 AAD</td>
      <td>21BG ATLS</td>
      <td>3ℓ + E<sub>T</sub>, Tchi1n2F, wino cross section, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 300</td>
      <td>95</td>
      <td>11 AAD</td>
      <td>21BG ATLS</td>
      <td>3ℓ + E<sub>T</sub>, Tchi1n2F, wino cross section, m<sub>χ̃<sub>0</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = m<sub>Z</sub></td>
    </tr>
    <tr>
      <td>&gt; 240</td>
      <td>95</td>
      <td>11 AAD</td>
      <td>21BG ATLS</td>
      <td>3ℓ + E<sub>T</sub>, Tchi1n2F, wino cross section, m<sub>χ̃<sub>0</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 10 GeV</td>
    </tr>
    <tr>
      <td>&gt; 195</td>
      <td>95</td>
      <td>11 AAD</td>
      <td>21BG ATLS</td>
      <td>3ℓ + E<sub>T</sub>, Tchi1n2Ga, higgsino cross section, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 10 GeV</td>
    </tr>
    <tr>
      <td>&gt; 190</td>
      <td>95</td>
      <td>11 AAD</td>
      <td>21BG ATLS</td>
      <td>3ℓ + E<sub>T</sub>, Tchi1n2E, wino cross section, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 1600</td>
      <td>95</td>
      <td>12 AAD</td>
      <td>21Y ATLS</td>
      <td>≥ 4ℓ, RPV Tchi1n2l with χ̃<sub>1</sub><sup>0</sup> → ℓ<sup>±</sup>ℓ<sup>∓</sup>ν, λ<sub>12k</sub> ≠ 0, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 1200 GeV</td>
    </tr>
    <tr>
      <td>&gt; 1100</td>
      <td>95</td>
      <td>12 AAD</td>
      <td>21Y ATLS</td>
      <td>≥ 4ℓ, RPV Tchi1n2l with χ̃<sub>1</sub><sup>0</sup> → ℓ<sup>±</sup>ℓ<sup>∓</sup>ν, λ<sub>133</sub> ≠ 0, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 1000 GeV</td>
    </tr>
    <tr>
      <td>&gt; 750</td>
      <td>95</td>
      <td>13 SIRUNYAN</td>
      <td>21M CMS</td>
      <td>ℓ<sup>±</sup>ℓ<sup>∓</sup> + E<sub>T</sub>, Tchi1n2F, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> &lt; 100 GeV</td>
    </tr>
    <tr>
      <td>none 400-820</td>
      <td>95</td>
      <td>14 TUMASYAN</td>
      <td>21C CMS</td>
      <td>1 ℓ<sup>±</sup> + 2b-jets + E<sub>T</sub>, Tchi1n2E, χ̃<sub>1</sub><sup>0</sup> = 200 GeV</td>
    </tr>
    <tr>
      <td>none 160-820</td>
      <td>95</td>
      <td>14 TUMASYAN</td>
      <td>21C CMS</td>
      <td>1 ℓ<sup>±</sup> + 2b-jets + E<sub>T</sub>, Tchi1n2E, χ̃<sub>1</sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 380</td>
      <td>95</td>
      <td>15 AAD</td>
      <td>20AN ATLS</td>
      <td>2γ + E<sub>T</sub>, Tn1n1A, GMSB</td>
    </tr>
    <tr>
      <td>&gt; 193</td>
      <td>95</td>
      <td>16 AAD</td>
      <td>20I ATLS</td>
      <td>2ℓ (soft), jets, E<sub>T</sub>; Tchi1n2Ga, higgsino, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 9.3 GeV</td>
    </tr>
    <tr>
      <td>&gt; 240</td>
      <td>95</td>
      <td>17 AAD</td>
      <td>20I ATLS</td>
      <td>2ℓ (soft), jets, E<sub>T</sub>; Tchi1n2Fb, wino, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 7 GeV</td>
    </tr>
    <tr>
      <td>&gt; 345</td>
      <td>95</td>
      <td>18 AAD</td>
      <td>20K ATLS</td>
      <td>3ℓ + E<sub>T</sub>, Tchi1n2F, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 740</td>
      <td>95</td>
      <td>19 AAD</td>
      <td>20R ATLS</td>
      <td>1ℓ + 2b-jets + E<sub>T</sub>, Tchi1n2E, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 290</td>
      <td>95</td>
      <td>20 SIRUNYAN</td>
      <td>20AU CMS</td>
      <td>soft τ + jet + E<sub>T</sub>, Tchi1n2D, wino, m<sub>χ̃<sub>±</sub></sub> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 50 GeV</td>
    </tr>
    <tr>
      <td>&gt; 680</td>
      <td>95</td>
      <td>21 AABOUD</td>
      <td>19AU ATL</td>
      <td>0, 1, 2 or more ℓ, H (→ γγ, bb, WW*, ZZ*, ττ) (various searches), Tchi1n2E, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 112</td>
      <td>95</td>
      <td>22 SIRUNYAN</td>
      <td>19BU CMS</td>
      <td>pp → χ̃<sub>1</sub><sup>±</sup>χ̃<sub>2</sub><sup>0</sup> + 2 jets, χ̃<sub>2</sub><sup>0</sup> → ℓ<sup>+</sup>ℓ<sup>-</sup>χ̃<sub>1</sub><sup>0</sup>, heavy sleptons, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 1 GeV, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> = m<sub>χ̃<sub>1</sub></sub><sup>±</sup></td>
    </tr>
    <tr>
      <td>&gt; 215</td>
      <td>95</td>
      <td>22 SIRUNYAN</td>
      <td>19BU CMS</td>
      <td>pp → χ̃<sub>1</sub><sup>±</sup>χ̃<sub>2</sub><sup>0</sup> + 2 jets, χ̃<sub>2</sub><sup>0</sup> → ℓ<sup>+</sup>ℓ<sup>-</sup>χ̃<sub>1</sub><sup>0</sup>, heavy sleptons, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 30 GeV, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> = m<sub>χ̃<sub>1</sub></sub><sup>±</sup></td>
    </tr>
    <tr>
      <td>&gt; 760</td>
      <td>95</td>
      <td>23 AABOUD</td>
      <td>18AY ATLS</td>
      <td>2τ + E<sub>T</sub>, Tchi1n2D and τ̃L-only, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt;1125</td>
      <td>95</td>
      <td>24 AABOUD</td>
      <td>18BT ATLS</td>
      <td>2,3ℓ + E<sub>T</sub>, Tchi1n2C, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 580</td>
      <td>95</td>
      <td>25 AABOUD</td>
      <td>18BT ATLS</td>
      <td>2,3ℓ + E<sub>T</sub>, Tchi1n2F, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>none 130-230, 290-880</td>
      <td>95</td>
      <td>26 AABOUD</td>
      <td>18CK ATLS</td>
      <td>2H (→ bb) + E<sub>T</sub>, Tn1n1A, GMSB</td>
    </tr>
    <tr>
      <td>none 220-600</td>
      <td>95</td>
      <td>27 AABOUD</td>
      <td>18CO ATLS</td>
      <td>2,3ℓ + E<sub>T</sub>, recursive jigsaw, Tchi1n2F, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 145</td>
      <td>95</td>
      <td>28 AABOUD</td>
      <td>18R ATLS</td>
      <td>2ℓ (soft) + E<sub>T</sub>, Tchi1n2G, higgsino, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 5 GeV</td>
    </tr>
    <tr>
      <td>&gt; 175</td>
      <td>95</td>
      <td>29 AABOUD</td>
      <td>18R ATLS</td>
      <td>2ℓ (soft) + E<sub>T</sub>, Tchi1n2F, wino, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 10 GeV</td>
    </tr>
    <tr>
      <td>&gt;1060</td>
      <td>95</td>
      <td>30 AABOUD</td>
      <td>18U ATLS</td>
      <td>2 γ + E<sub>T</sub>, GGM, Tchi1chi1A, any NLSP mass</td>
    </tr>
    <tr>
      <td>&gt; 167</td>
      <td>95</td>
      <td>31 SIRUNYAN</td>
      <td>18AJ CMS</td>
      <td>2ℓ (soft) + E<sub>T</sub>, Tchi1n2G, higgsino, m<sub>χ̃<sub>2</sub></sub><sup>0</sup> - m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 15 GeV</td>
    </tr>
    <tr>
      <td>&gt; 710</td>
      <td>95</td>
      <td>32 SIRUNYAN</td>
      <td>18DP CMS</td>
      <td>2τ + E<sub>T</sub>, Tchi1n2D, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>none 220-490</td>
      <td>95</td>
      <td>33 SIRUNYAN</td>
      <td>17AW CMS</td>
      <td>1ℓ + 2 b-jets + E<sub>T</sub>, Tchi1n2E, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 600</td>
      <td>95</td>
      <td>34 AAD</td>
      <td>16AA ATLS</td>
      <td>3,4ℓ + E<sub>T</sub>, Tn2n3A, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> = 0 GeV</td>
    </tr>
    <tr>
      <td>&gt; 670</td>
      <td>95</td>
      <td>34 AAD</td>
      <td>16AA ATLS</td>
      <td>3,4ℓ + E<sub>T</sub>, Tn2n3B, m<sub>χ̃<sub>1</sub></sub><sup>0</sup> &lt; 200 GeV</td>
    </tr>
  </tbody>
</table>