For $m_{\chi_0} = 20$ GeV

<table><thead><tr><th>VALUE (nb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 0.03</td><td>90</td><td>1 UCHIDA</td><td>14</td><td>XMAS 129<sup>Xe</sup>, inelastic</td></tr><tr><td>&lt; 0.08</td><td>90</td><td>2 ANGLOHER</td><td>02</td><td>CRES Al</td></tr><tr><td></td><td></td><td>3 BENOIT</td><td>00</td><td>EDEL Ge</td></tr><tr><td>&lt; 0.04</td><td>95</td><td>4 KLIMENKO</td><td>98</td><td>CNTR 73<sup>Ge</sup>, inel.</td></tr><tr><td>&lt; 0.8</td><td></td><td>ALESSAND...</td><td>96</td><td>CNTR O</td></tr><tr><td>&lt; 6</td><td></td><td>ALESSAND...</td><td>96</td><td>CNTR Te</td></tr><tr><td>&lt; 0.02</td><td>90</td><td>5 BELLI</td><td>96</td><td>CNTR 129<sup>Xe</sup>, inel.</td></tr><tr><td></td><td></td><td>6 BELLI</td><td>96c</td><td>CNTR 129<sup>Xe</sup></td></tr><tr><td>&lt; 4 &times; 10<sup>-3</sup></td><td>90</td><td>7 BERNABEI</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 0.3</td><td>90</td><td>7 BERNABEI</td><td>96</td><td>CNTR I</td></tr><tr><td>&lt; 0.2</td><td>95</td><td>8 SARSA</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 0.015</td><td>90</td><td>9 SMITH</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 0.05</td><td>95</td><td>10 GARCIA</td><td>95</td><td>CNTR Natural Ge</td></tr><tr><td>&lt; 0.1</td><td>95</td><td>QUENBY</td><td>95</td><td>CNTR Na</td></tr><tr><td>&lt;90</td><td>90</td><td>11 SNOWDEN...</td><td>95</td><td>MICA 16<sup>O</sup></td></tr><tr><td>&lt; 4 &times; 10<sup>3</sup></td><td>90</td><td>11 SNOWDEN...</td><td>95</td><td>MICA 39<sup>K</sup></td></tr><tr><td>&lt; 0.7</td><td>90</td><td>BACCI</td><td>92</td><td>CNTR Na</td></tr><tr><td>&lt; 0.12</td><td>90</td><td>12 REUSSER</td><td>91</td><td>CNTR Natural Ge</td></tr><tr><td>&lt; 0.06</td><td>95</td><td>CALDWELL</td><td>88</td><td>CNTR Natural Ge</td></tr></tbody></table>

¹ UCHIDA 14 limit is for inelastic scattering $\chi^0 + 129^{Xe}* \to \chi^0 + 129^{Xe}*$ (39.58 keV).

² ANGLOHER 02 limit is for spin-dependent WIMP-Aluminum cross section.

³ BENOIT 00 find four event categories in Ge detectors and suggest that low-energy surface nuclear recoils can explain anomalous events reported by UKDMC and Saclay Nal experiments.

⁴ KLIMENKO 98 limit is for inelastic scattering $\chi^0 73^{Ge} \to \chi^0 73^{Ge}*$ (13.26 keV).

⁵ BELLI 96 limit for inelastic scattering $\chi^0 129^{Xe} \to \chi^0 129^{Xe}*$ (39.58 keV).

⁶ BELLI 96C use background subtraction and obtain $\sigma < 150$ pb (< 1.5 fb) (90% CL) for spin-dependent (independent) $\chi^0$-proton cross section. The confidence level is from R. Bernabei, private communication, May 20, 1999.

⁷ BERNABEI 96 use pulse shape discrimination to enhance the possible signal. The limit here is from R. Bernabei, private communication, September 19, 1997.

⁸ SARSA 96 search for annual modulation of WIMP signal. See SARSA 97 for details of the analysis. The limit here is from M.L. Sarsa, private communication, May 26, 1997.

⁹ SMITH 96 use pulse shape discrimination to enhance the possible signal. A dark matter density of 0.4 GeV cm$^{-3}$ is assumed.

¹⁰ GARCIA 95 limit is from the event rate. A weaker limit is obtained from searches for diurnal and annual modulation.

¹¹ SNOWDEN-IFFT 95 look for recoil tracks in an ancient mica crystal. Similar limits are also given for ²⁷Al and ²⁸Si. See COLLAR 96 and SNOWDEN-IFFT 96 for discussion on potential backgrounds.

¹² REUSSER 91 limit here is changed from published (0.04) after reanalysis by authors. J.L. Vuilleumier, private communication, March 29, 1996.

For $m_{\chi_0} = 100$ GeV

<table><thead><tr><th>VALUE (nb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 3.3 &times; 10<sup>-6</sup></td><td>90</td><td>1 APRILE</td><td>21A</td><td>XE1T 129<sup>Xe</sup>, inelastic</td></tr><tr><td>&lt; 3 &times; 10<sup>-3</sup></td><td>90</td><td>2 UCHIDA</td><td>14</td><td>XMAS 129<sup>Xe</sup>, inelastic</td></tr><tr><td>&lt; 0.3</td><td>90</td><td>3 ANGLOHER</td><td>02</td><td>CRES Al</td></tr><tr><td></td><td></td><td>4 BELLI</td><td>02</td><td>RVUE</td></tr><tr><td></td><td></td><td>5 BERNABEI</td><td>02c</td><td>DAMA</td></tr><tr><td></td><td></td><td>6 GREEN</td><td>02</td><td>RVUE</td></tr><tr><td></td><td></td><td>7 ULLIO</td><td>01</td><td>RVUE</td></tr><tr><td></td><td></td><td>8 BENOIT</td><td>00</td><td>EDEL Ge</td></tr><tr><td>&lt; 4 &times; 10<sup>-3</sup></td><td>90</td><td>9 BERNABEI</td><td>00d</td><td>129<sup>Xe</sup>, inelastic</td></tr><tr><td></td><td></td><td>10 AMBROSIO</td><td>99</td><td>MCRO</td></tr><tr><td></td><td></td><td>11 BRHLIK</td><td>99</td><td>RVUE</td></tr><tr><td>&lt; 8 &times; 10<sup>-3</sup></td><td>95</td><td>12 KLIMENKO</td><td>98</td><td>CNTR 73<sup>Ge</sup>, inelastic</td></tr><tr><td>&lt; 0.08</td><td>95</td><td>13 KLIMENKO</td><td>98</td><td>CNTR 73<sup>Ge</sup>, inelastic</td></tr><tr><td>&lt; 4</td><td></td><td>ALESSAND...</td><td>96</td><td>CNTR O</td></tr><tr><td>&lt;25</td><td></td><td>ALESSAND...</td><td>96</td><td>CNTR Te</td></tr><tr><td>&lt; 6 &times; 10<sup>-3</sup></td><td>90</td><td>14 BELLI</td><td>96</td><td>CNTR 129<sup>Xe</sup>, inelastic</td></tr><tr><td></td><td></td><td>15 BELLI</td><td>96c</td><td>CNTR 129<sup>Xe</sup></td></tr><tr><td>&lt; 1 &times; 10<sup>-3</sup></td><td>90</td><td>16 BERNABEI</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 0.3</td><td>90</td><td>16 BERNABEI</td><td>96</td><td>CNTR I</td></tr><tr><td>&lt; 0.7</td><td>95</td><td>17 SARSA</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 0.03</td><td>90</td><td>18 SMITH</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 0.8</td><td>90</td><td>18 SMITH</td><td>96</td><td>CNTR I</td></tr><tr><td>&lt; 0.35</td><td>95</td><td>19 GARCIA</td><td>95</td><td>CNTR Natural Ge</td></tr><tr><td>&lt; 0.6</td><td>95</td><td>QUENBY</td><td>95</td><td>CNTR Na</td></tr><tr><td>&lt; 3</td><td>95</td><td>QUENBY</td><td>95</td><td>CNTR I</td></tr><tr><td>&lt; 1.5 &times; 10<sup>2</sup></td><td>90</td><td>20 SNOWDEN...</td><td>95</td><td>MICA 16<sup>O</sup></td></tr><tr><td>&lt; 4 &times; 10<sup>2</sup></td><td>90</td><td>20 SNOWDEN...</td><td>95</td><td>MICA 39<sup>K</sup></td></tr><tr><td>&lt; 0.08</td><td>90</td><td>21 BECK</td><td>94</td><td>CNTR 76<sup>Ge</sup></td></tr><tr><td>&lt; 2.5</td><td>90</td><td>BACCI</td><td>92</td><td>CNTR Na</td></tr><tr><td>&lt; 3</td><td>90</td><td>BACCI</td><td>92</td><td>CNTR I</td></tr><tr><td>&lt; 0.9</td><td>90</td><td>22 REUSSER</td><td>91</td><td>CNTR Natural Ge</td></tr><tr><td>&lt; 0.7</td><td>95</td><td>CALDWELL</td><td>88</td><td>CNTR Natural Ge</td></tr></tbody></table>

¹ APRILE 21A search for inelastic DM scatter off ¹²⁹Xe nuclei with 0.83 t yr exposure. No signal observed. Limits placed in $\sigma(\chi_Xe)$ vs. m(DM) plane for WIMP mass between 20 GeV and 10 TeV.

² UCHIDA 14 limit is for inelastic scattering $\chi^0 + 129^{Xe}* \to \chi^0 + 129^{Xe}*$ (39.58 keV).

³ ANGLOHER 02 limit is for spin-dependent WIMP-Aluminum cross section.

⁴ BELLI 02 discusses dependence of the extracted WIMP cross section on the assumptions of the galactic halo structure.

⁵ BERNABEI 02c analyze the DAMA data in the scenario in which $\chi^0$ scatters into a slightly heavier state as discussed by SMITH 01.

⁶ GREEN 02 discusses dependence of extracted WIMP cross section limits on the assumptions of the galactic halo structure.

⁷ ULLIO 01 disfavor the possibility that the BERNABEI 99 signal is due to spin-dependent WIMP coupling.

⁸ BENOIT 00 find four event categories in Ge detectors and suggest that low-energy surface nuclear recoils can explain anomalous events reported by UKDMC and Saclay Nal experiments.

⁹ BERNABEI 00d limit is for inelastic scattering $\chi^{0}_{129^{Xe}} \to \chi^{0}_{129^{Xe}}$ (39.58 keV).

¹⁰ AMBROSIO 99 search for upgoing muon events induced by neutrinos originating from WIMP annihilations in the Sun and Earth.

¹¹ BRHLIK 99 discuss the effect of astrophysical uncertainties on the WIMP interpretation of the BERNABEI 99 signal.

¹² KLIMENKO 98 limit is for inelastic scattering $\chi^0 73^{Ge} \to \chi^0 73^{Ge}*$ (13.26 keV).

¹³ KLIMENKO 98 limit is for inelastic scattering $\chi^0 73^{Ge} \to \chi^0 73^{Ge}*$ (66.73 keV).

¹⁴ BELLI 96 limit for inelastic scattering $\chi^0 129^{Xe} \to \chi^0 129^{Xe}*$ (39.58 keV).

¹⁵ BELLI 96c use background subtraction and obtain $\sigma < 0.35$ pb (< 0.15 fb) (90% CL) for spin-dependent (independent) $\chi^0$-proton cross section. The confidence level is from R. Bernabei, private communication, May 20, 1999.

¹⁶ BERNABEI 96 use pulse shape discrimination to enhance the possible signal. The limit here is from R. Bernabei, private communication, September 19, 1997.

¹⁷ SARSA 96 search for annual modulation of WIMP signal. See SARSA 97 for details of the analysis. The limit here is from M.L. Sarsa, private communication, May 26, 1997.

¹⁸ SMITH 96 use pulse shape discrimination to enhance the possible signal. A dark matter density of 0.4 GeV cm$^{-3}$ is assumed.

¹⁹ GARCIA 95 limit is from the event rate. A weaker limit is obtained from searches for diurnal and annual modulation.

²⁰ SNOWDEN-IFFT 95 look for recoil tracks in an ancient mica crystal. Similar limits are also given for ²⁷Al and ²⁸Si. See COLLAR 96 and SNOWDEN-IFFT 96 for discussion on potential backgrounds.

²¹ BECK 94 uses enriched ⁷⁶Ge (86% purity).

²² REUSSER 91 limit here is changed from published (0.3) after reanalysis by authors. J.L. Vuilleumier, private communication, March 29, 1996.

For $m_{\chi_0} = 1$ TeV

<table><thead><tr><th>VALUE (nb)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 0.03</td><td>90</td><td>1 UCHIDA</td><td>14</td><td>XMAS 129<sup>Xe</sup>, inelastic</td></tr><tr><td>&lt; 3</td><td>90</td><td>2 ANGLOHER</td><td>02</td><td>CRES Al</td></tr><tr><td></td><td></td><td>3 BENOIT</td><td>00</td><td>EDEL Ge</td></tr><tr><td></td><td></td><td>4 BERNABEI</td><td>99d</td><td>CNTR SIMP</td></tr><tr><td></td><td></td><td>5 DERBIN</td><td>99</td><td>CNTR SIMP</td></tr><tr><td>&lt; 0.06</td><td>95</td><td>6 KLIMENKO</td><td>98</td><td>CNTR 73<sup>Ge</sup>, inel.</td></tr><tr><td>&lt; 0.4</td><td>95</td><td>7 KLIMENKO</td><td>98</td><td>CNTR 73<sup>Ge</sup>, inel.</td></tr><tr><td>&lt; 40</td><td></td><td>ALESSAND...</td><td>96</td><td>CNTR O</td></tr><tr><td>&lt;700</td><td></td><td>ALESSAND...</td><td>96</td><td>CNTR Te</td></tr><tr><td>&lt; 0.05</td><td>90</td><td>8 BELLI</td><td>96</td><td>CNTR 129<sup>Xe</sup>, inel.</td></tr><tr><td>&lt; 1.5</td><td>90</td><td>9 BELLI</td><td>96</td><td>CNTR 129<sup>Xe</sup>, inel.</td></tr><tr><td></td><td></td><td>10 BELLI</td><td>96c</td><td>CNTR 129<sup>Xe</sup></td></tr><tr><td>&lt; 0.01</td><td>90</td><td>11 BERNABEI</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 9</td><td>90</td><td>11 BERNABEI</td><td>96</td><td>CNTR I</td></tr><tr><td>&lt; 7</td><td>95</td><td>12 SARSA</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 0.3</td><td>90</td><td>13 SMITH</td><td>96</td><td>CNTR Na</td></tr><tr><td>&lt; 6</td><td>90</td><td>13 SMITH</td><td>96</td><td>CNTR I</td></tr><tr><td>&lt; 6</td><td>95</td><td>14 GARCIA</td><td>95</td><td>CNTR Natural Ge</td></tr><tr><td>&lt; 8</td><td>95</td><td>QUENBY</td><td>95</td><td>CNTR Na</td></tr><tr><td>&lt; 50</td><td>95</td><td>QUENBY</td><td>95</td><td>CNTR I</td></tr><tr><td>&lt;700</td><td>90</td><td>15 SNOWDEN-...</td><td>95</td><td>MICA 16<sup>O</sup></td></tr><tr><td>&lt; 1 &times; 10<sup>3</sup></td><td>90</td><td>15 SNOWDEN-...</td><td>95</td><td>MICA 39<sup>K</sup></td></tr><tr><td>&lt; 0.8</td><td>90</td><td>16 BECK</td><td>94</td><td>CNTR 76<sup>Ge</sup></td></tr><tr><td>&lt; 30</td><td>90</td><td>BACCI</td><td>92</td><td>CNTR Na</td></tr><tr><td>&lt; 30</td><td>90</td><td>BACCI</td><td>92</td><td>CNTR I</td></tr><tr><td>&lt; 15</td><td>90</td><td>17 REUSSER</td><td>91</td><td>CNTR Natural Ge</td></tr><tr><td>&lt; 6</td><td>95</td><td>CALDWELL</td><td>88</td><td>CNTR Natural Ge</td></tr></tbody></table>

¹ UCHIDA 14 limit is for inelastic scattering $\chi^0 + 129^{Xe}* \to \chi^0 + 129^{Xe}*$ (39.58 keV).

² ANGLOHER 02 limit is for spin-dependent WIMP-Aluminum cross section.

³ BENOIT 00 find four event categories in Ge detectors and suggest that low-energy surface nuclear recoils can explain anomalous events reported by UKDMC and Saclay Nal experiments.

⁴ BERNABEI 99d search for SIMPs (Strongly Interacting Massive Particles) in the mass range 10³⁻¹⁰⁶ GeV. See their Fig. 3 for cross-section limits.

⁵ DERBIN 99 search for SIMPs (Strongly Interacting Massive Particles) in the mass range 10²⁻¹⁰⁴ GeV. See their Fig. 3 for cross-section limits.

⁶ KLIMENKO 98 limit is for inelastic scattering $\chi^0 73^{Ge} \to \chi^0 73^{Ge}*$ (13.26 keV).

⁷ KLIMENKO 98 limit is for inelastic scattering $\chi^0 73^{Ge} \to \chi^0 73^{Ge}*$ (66.73 keV).

⁸ BELLI 96 limit for inelastic scattering $\chi^0 129^{Xe} \to \chi^0 129^{Xe}*$ (39.58 keV).

⁹ BELLI 96 limit for inelastic scattering $\chi^0 129^{Xe} \to \chi^0 129^{Xe}*$ (236.14 keV).

¹⁰ BELLI 96c use background subtraction and obtain $\sigma < 0.7$ pb (< 0.15 fb) (90% CL) for spin-dependent (independent) $\chi^0$-proton cross section. The confidence level is from R. Bernabei, private communication, May 20, 1999.

¹¹ BERNABEI 96 use pulse shape discrimination to enhance the possible signal. The limit here is from R. Bernabei, private communication, September 19, 1997.

¹² SARSA 96 search for annual modulation of WIMP signal. See SARSA 97 for details of the analysis. The limit here is from M.L. Sarsa, private communication, May 26, 1997.
See key on page 1171

Searches Particle Listings
WIMP and Dark Matter Searches

<table><thead><tr><th></th><th></th><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td>&lt;2</td><td>× 10<sup>-26</sup></td><td>95</td><td>9</td><td>9 LAVIS</td><td>23</td><td>b&#773; + 2HDM+s, m&lt;1000 GeV</td></tr><tr><td>&lt;1.2</td><td>× 10<sup>-26</sup></td><td>95</td><td>10</td><td>ABDALLA</td><td>22</td><td>HESS DM annihilation to gamma rays</td></tr><tr><td></td><td></td><td></td><td>11</td><td>ALBERT</td><td>22A</td><td>ANTR PeV-scale DM search</td></tr><tr><td>&lt;1</td><td>× 10<sup>-27</sup></td><td></td><td>12</td><td>CHAN</td><td>22</td><td>DM annihilation from Omega Centauri X-rays</td></tr><tr><td>&lt;3</td><td>× 10<sup>-26</sup></td><td></td><td>13</td><td>EGOROV</td><td>22</td><td>DM annihilation to radio waves from M31</td></tr><tr><td></td><td></td><td></td><td>14</td><td>MANCONI</td><td>22</td><td>polarized synchrotron emission from DM annihilation via Planck</td></tr><tr><td>&lt;5</td><td>× 10<sup>-24</sup></td><td>95</td><td>15</td><td>ABDALLAH</td><td>21</td><td>HESS WIMP annihilation in dwarf irregular galaxy</td></tr><tr><td></td><td></td><td></td><td>16</td><td>CIRELLI</td><td>21</td><td>light DM annihilation producing X-rays</td></tr><tr><td></td><td></td><td></td><td>17</td><td>JOHN</td><td>21</td><td>cosmic positron spectra limits on leptophilic DM</td></tr><tr><td>&lt;2.5</td><td>× 10<sup>-27</sup></td><td>95</td><td>18</td><td>ABAZAJIAN</td><td>20</td><td>FLAT γ from galactic center</td></tr><tr><td></td><td></td><td></td><td>19</td><td>ABDALLAH</td><td>20</td><td>HESS WIMP annihilation in dwarf satellite galaxies</td></tr><tr><td>&lt;1.2</td><td>× 10<sup>-24</sup></td><td>90</td><td>20</td><td>ABE</td><td>20G</td><td>SKAM WIMP annihilation to neutrinos</td></tr><tr><td>&lt;2.2</td><td>× 10<sup>-24</sup></td><td>95</td><td>21</td><td>ALBERT</td><td>20</td><td>HAWC WIMP annihilation to γ</td></tr><tr><td>&lt;5</td><td>× 10<sup>-24</sup></td><td>90</td><td>22</td><td>ALBERT</td><td>20A</td><td>ANTR WIMP annihilation to νs in galactic center</td></tr><tr><td>&lt;1</td><td>× 10<sup>-23</sup></td><td>90</td><td>23</td><td>ALBERT</td><td>20C</td><td>ANTR Ames IceCube search for WIMP annihilation to νs</td></tr><tr><td>&lt;8</td><td>× 10<sup>-26</sup></td><td></td><td>24</td><td>ALVAREZ</td><td>20</td><td>FLAT dwarf spheroidal; J-distribution</td></tr><tr><td>&lt;2</td><td>× 10<sup>-26</sup></td><td>90</td><td>25</td><td>HOOF</td><td>20</td><td>FLAT WIMP annihilation to γ</td></tr><tr><td></td><td></td><td></td><td>26</td><td>MAZZIOTTA</td><td>20</td><td>FLAT DM annihilation in Sun to γ</td></tr><tr><td></td><td></td><td></td><td>27</td><td>ABEYSEKARA</td><td>19</td><td>HAWC DM annihilation to γs within galactic substructure</td></tr><tr><td>&lt;0.8</td><td>× 10<sup>-22</sup></td><td>95</td><td>28</td><td>ALBERT</td><td>19B</td><td>HAWC annihilation/decay to γ in M31</td></tr><tr><td>&lt;4</td><td>× 10<sup>-26</sup></td><td>95</td><td>29</td><td>CHEUNG</td><td>19</td><td>EDGS χχ → e<sup>+</sup>e<sup>-</sup> and b&#773;</td></tr><tr><td>&lt;7</td><td>× 10<sup>-27</sup></td><td>95</td><td>30</td><td>DI-MAURO</td><td>19</td><td>FLAT Fermi-LAT M31 and M33</td></tr><tr><td></td><td></td><td></td><td>31</td><td>JOHNSON</td><td>19</td><td>FLAT P-wave DM; Fermi-LAT</td></tr><tr><td>&lt;2</td><td>× 10<sup>-26</sup></td><td>95</td><td>32</td><td>LI</td><td>19D</td><td>FLAT χχ → γ</td></tr><tr><td>&lt;1</td><td>× 10<sup>-32</sup></td><td></td><td>33</td><td>NG</td><td>19</td><td>sterile ν decay/annihilation</td></tr><tr><td></td><td></td><td></td><td>34</td><td>QUEIROZ</td><td>19</td><td>semi-annihilating DM</td></tr><tr><td>&lt;4</td><td>× 10<sup>-28</sup></td><td>95</td><td>35</td><td>ABDALLAH</td><td>18</td><td>HESS X<sup>0</sup>χ<sup>0</sup> → γX; galactic halo</td></tr><tr><td>&lt;1</td><td>× 10<sup>-23</sup></td><td>95</td><td>36</td><td>AHNEN</td><td>18</td><td>MGIC X<sup>0</sup>χ<sup>0</sup> → γX; Ursa Major II</td></tr><tr><td>&lt;1</td><td>× 10<sup>-22</sup></td><td>95</td><td>37</td><td>ALBERT</td><td>18B</td><td>HAWC X<sup>0</sup>χ<sup>0</sup> → γX; Andromeda</td></tr><tr><td>&lt;1</td><td>× 10<sup>-26</sup></td><td>95</td><td>38</td><td>CHANG</td><td>18A</td><td>χχ → b&#773; → γ</td></tr><tr><td></td><td></td><td></td><td>39</td><td>LISANTI</td><td>18</td><td>THEO Fermi, γ; galaxy groups</td></tr><tr><td></td><td></td><td></td><td>40</td><td>MAZZIOTTA</td><td>18</td><td>FLAT Fermi-LAT CRE data</td></tr><tr><td>&lt;1.2</td><td>× 10<sup>-23</sup></td><td>95</td><td>41</td><td>AARTSEN</td><td>17C</td><td>ICCB χχ → neutrinos</td></tr><tr><td>&lt;1</td><td>× 10<sup>-23</sup></td><td>90</td><td>42</td><td>ALBERT</td><td>17A</td><td>ANTR ν, DM annihilation</td></tr><tr><td>&lt;1.32</td><td>× 10<sup>-25</sup></td><td>95</td><td>43</td><td>ARCHAMBAU..17</td><td>17</td><td>VRTS γ dwarf galaxies</td></tr><tr><td>&lt;7</td><td>× 10<sup>-21</sup></td><td>90</td><td>44</td><td>AVRORIN</td><td>17</td><td>BAIK cosmic ν</td></tr><tr><td>&lt;1</td><td>× 10<sup>-28</sup></td><td></td><td>45</td><td>BOUDAUD</td><td>17</td><td>MeV DM to e<sup>+</sup>e<sup>-</sup></td></tr><tr><td></td><td></td><td></td><td>46</td><td>AARTSEN</td><td>16D</td><td>ICCB ν, galactic center</td></tr><tr><td>&lt;6</td><td>× 10<sup>-26</sup></td><td>95</td><td>47</td><td>ABDALLAH</td><td>13</td><td>HESS Central Galactic Halo</td></tr><tr><td>&lt;1</td><td>× 10<sup>-27</sup></td><td>95</td><td>48</td><td>ABDALLAH</td><td>16A</td><td>HESS WIMP+WIMP → γγ; galactic center</td></tr><tr><td>&lt;3</td><td>× 10<sup>-26</sup></td><td>95</td><td>49</td><td>AHNEN</td><td>16</td><td>MGFL Satellite galaxy, m(WIMP)=100 GeV</td></tr><tr><td>&lt;1.9</td><td>× 10<sup>-21</sup></td><td>90</td><td>50</td><td>AVRORIN</td><td>16</td><td>BAIK νs from galactic center</td></tr><tr><td>&lt;3</td><td>× 10<sup>-26</sup></td><td>95</td><td>51</td><td>CAPUTO</td><td>16</td><td>FLAT small Magellanic cloud</td></tr><tr><td>&lt;1</td><td>× 10<sup>-25</sup></td><td>95</td><td>52</td><td>FORNASA</td><td>16</td><td>Fermi-LAT γ-ray anisotropy</td></tr><tr><td>&lt;5</td><td>× 10<sup>-27</sup></td><td></td><td>53</td><td>LEITE</td><td>16</td><td>FLAT WIMP, radio</td></tr><tr><td>&lt;2</td><td>× 10<sup>-26</sup></td><td>95</td><td>54</td><td>LI</td><td>16</td><td>FLAT dwarf galaxies</td></tr><tr><td>&lt;1</td><td>× 10<sup>-25</sup></td><td>95</td><td>55</td><td>LI</td><td>16A</td><td>FLAT Fermi-LAT; M31</td></tr><tr><td>&lt;1</td><td>× 10<sup>-26</sup></td><td></td><td>56</td><td>LIANG</td><td>16</td><td>FLAT Fermi-LAT, gamma line</td></tr><tr><td>&lt;1</td><td>× 10<sup>-25</sup></td><td>95</td><td>57</td><td>LU</td><td>16</td><td>FLAT Fermi-LAT and AMS-02</td></tr><tr><td>&lt;1</td><td>× 10<sup>-23</sup></td><td>95</td><td>58</td><td>SHIRASAKI</td><td>16</td><td>FLAT extra galaxy</td></tr><tr><td></td><td></td><td></td><td>59</td><td>AARTSEN</td><td>15C</td><td>ICCB ν, Galactic halo</td></tr><tr><td></td><td></td><td></td><td>60</td><td>AARTSEN</td><td>15E</td><td>ICCB ν, Galactic center</td></tr><tr><td></td><td></td><td></td><td>61</td><td>ABRAMOWSKI</td><td>11</td><td>HESS Galactic center</td></tr><tr><td></td><td></td><td></td><td>62</td><td>ACKERMANN</td><td>15</td><td>FLAT monochromatic γ</td></tr><tr><td></td><td></td><td></td><td>63</td><td>ACKERMANN</td><td>15A</td><td>FLAT isotropic γ background</td></tr><tr><td></td><td></td><td></td><td>64</td><td>ACKERMANN</td><td>15B</td><td>FLAT Satellite galaxy</td></tr><tr><td></td><td></td><td></td><td>65</td><td>ADRIAN-MAR..15</td><td>ANTR ν, Galactic center</td><td></td></tr><tr><td>&lt;2.90</td><td>× 10<sup>-26</sup></td><td>95</td><td>66,67</td><td>ACKERMANN</td><td>14</td><td>FLAT Satellite galaxy, m = 10 GeV</td></tr><tr><td>&lt;1.84</td><td>× 10<sup>-25</sup></td><td>95</td><td>66,68</td><td>ACKERMANN</td><td>14</td><td>FLAT Satellite galaxy, m = 100 GeV</td></tr><tr><td>&lt;1.75</td><td>× 10<sup>-24</sup></td><td>95</td><td>66,68</td><td>ACKERMANN</td><td>14</td><td>FLAT Satellite galaxy, m = 1 TeV</td></tr><tr><td>&lt;4.52</td><td>× 10<sup>-24</sup></td><td>95</td><td>69</td><td>ALEKSIC</td><td>14</td><td>MGIC Segue 1, m = 1.35 TeV</td></tr><tr><td></td><td></td><td></td><td>70</td><td>AARTSEN</td><td>13C</td><td>ICCB Galaxies</td></tr><tr><td></td><td></td><td></td><td>71</td><td>ABRAMOWSKI</td><td>11</td><td>HESS Central Galactic Halo</td></tr><tr><td></td><td></td><td></td><td>72</td><td>ACKERMANN</td><td>13A</td><td>FLAT Galaxy</td></tr><tr><td></td><td></td><td></td><td>73</td><td>ABRAMOWSKI</td><td>12</td><td>HESS Fornax Cluster</td></tr><tr><td></td><td></td><td></td><td>74</td><td>ACKERMANN</td><td>12</td><td>FLAT Galaxy</td></tr><tr><td></td><td></td><td></td><td>75</td><td>ACKERMANN</td><td>12</td><td>FLAT Galaxy</td></tr><tr><td></td><td></td><td></td><td>76</td><td>ALIU</td><td>12</td><td>VRTS Segue 1</td></tr><tr><td>&lt;1</td><td>× 10<sup>-22</sup></td><td>90</td><td>77</td><td>ABBASI</td><td>11C</td><td>ICCB Galactic halo, m=1 TeV</td></tr><tr><td>&lt;3</td><td>× 10<sup>-25</sup></td><td>95</td><td>78</td><td>ABRAMOWSKI</td><td>11</td><td>HESS Near Galactic center, m=1 TeV</td></tr><tr><td>&lt;1</td><td>× 10<sup>-26</sup></td><td>95</td><td>79</td><td>ACKERMANN</td><td>11</td><td>FLAT Satellite galaxy, m=10 GeV</td></tr><tr><td>&lt;1</td><td>× 10<sup>-25</sup></td><td>95</td><td>79</td><td>ACKERMANN</td><td>11</td><td>FLAT Satellite galaxy, m=100 GeV</td></tr><tr><td>&lt;1</td><td>× 10<sup>-24</sup></td><td>95</td><td>79</td><td>ACKERMANN</td><td>11</td><td>FLAT Satellite galaxy, m=1 TeV</td></tr></tbody></table>

<footnote n="1">1 ABBASI 23A search for WIMP-WIMP annihilation to ν's. No signal observed. Require $\langle\sigma\cdot\nu\rangle < 10^{-24}$ cm$^3$/s for m(χ) ~ 10-10 × 10$^4$ GeV for various halo profiles.</footnote>

<footnote n="2">2 ABBASI 23B search for PeV-scale WIMP-WIMP annihilation to μ or b pairs. No signal observed. Require $\langle\sigma\cdot\nu\rangle < 10^{-22}$ cm$^3$/s for χχ → b$\bar{b}$ with m(χ) about 1 PeV or $\langle\sigma\cdot\nu\rangle < 10^{-23}$ cm$^3$/s for χχ → μ$^+$μ$^-$ with m(χ) about 1 PeV.</footnote>

<footnote n="3">3 ABE 23B search for WIMP-WIMP annihilation to γ in GC. No signal observed. Require $\langle\sigma\cdot\nu\rangle < 5 \times 10^{-28}$ cm$^3$/s for m(χ) = 1 TeV or $\langle\sigma\cdot\nu\rangle < 1 \times 10^{-25}$ cm$^3$/s for m(χ) = 100 TeV.</footnote>

<footnote n="4">4 ALBERT 23 search for WIMP pair annihilation to γ in galactic halo. No signal observed. Limits placed in $\langle\sigma\cdot\nu\rangle$ vs. mass (10-100 TeV) plane for various annihilation channels.</footnote>

<footnote n="5">5 CHENG 23A provide updated combined Fermi-LAT/DAMPE search for a gamma line from WIMP annihilation. No signal observed. Limits placed in $\langle\sigma\cdot\nu\rangle$ vs. mass (6-200 GeV) plane for various halo profiles.</footnote>

<footnote n="6">6 FOSTER 23 search for gamma ray line in Fermi-LAT data. No signal observed. Limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(χ) plane. For Higgsino DM limit see Fig. 12.</footnote>

<footnote n="7">7 GUO 23 search with Five-hundred-meter Aperture Spherical Radio Telescope for synchrotron emission radio signal of DM annihilation from dwarf spheroidal halo. No signal observed. Limits set in $\langle\sigma\cdot\nu\rangle$ vs. m(χ) plane for various annihilation final states.</footnote>

<footnote n="8">8 GUO 23A search in public IceCube data for DM annihilation to neutrinos. No signal observed. Limits placed in $\langle\sigma\cdot\nu\rangle$ vs m(χ) plane for various annihilation assumptions.</footnote>

<footnote n="9">9 LAVIS 23 search for 2HDM+s DM and generic spectra using MeerKAT. No signal observed. Limits placed in $\langle\sigma\cdot\nu\rangle$ vs mass (10-1000 GeV) plane for various annihilation channels.</footnote>

<footnote n="10">10 ABDALLA 22 search for WIMP annihilation in galactic center to gamma rays using HESS; no signal observed; limits set in mass vs $\langle\sigma\cdot\nu\rangle$ plane for dominant annihilation to WW or $\tau\bar{\tau}$. Limit here for $\tau\bar{\tau}$ channel 0.7 TeV mass.</footnote>

<footnote n="11">11 ALBERT 22A search for secluded PeV-scale DM annihilation to four final states; no signal detected; limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(χ) plane for m(χ): 6-6000 TeV for m(mediator) = 50, 250, and 1000 GeV.</footnote>

<footnote n="12">12 CHAN 22 derive a variety of limits on DM annihilation to various channels resulting in X-rays from dwarf galaxy Omega Centauri. Limits are very dependent on assumed DM density and diffusion coefficient. Quoted limit is for m(WIMP) = 100 GeV annihilating to WW with parameters as in Fig. 4.</footnote>

<footnote n="13">13 EGOROV 22 derives limits on DM annihilation to b$\bar{b}$ or $\tau\bar{\tau}$ via radio signals from M31; quoted limit from b$\bar{b}$ channel with LOFAR telescope as main data source, using parameters as in Fig. 10 (green curve) for m(χ) = 100 GeV.</footnote>

<footnote n="14">14 MANCONI 22 use polarized synchrotron emission data from Planck to constrain WIMP annihilation cross section in Galaxy; limits set in $\langle\sigma\cdot\nu\rangle$ vs. m(DM) plane.</footnote>

<footnote n="15">15 ABDALLAH 21 search for WIMP-WIMP annihilation into 2 monoenergetic γ rays in WLM dwarf irregular galaxy using HESS data. No signal. Limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(WIMP) plane for a mass of 370 GeV.</footnote>

<footnote n="16">16 CIRELLI 21 derive limits on light DM annihilation to e$\bar{e}$, μ$\mu$, ππ that then produce X-rays using data published by INTEGRAL telescope. Limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(DM) plane for m(DM) = 1-5000 MeV.</footnote>

<footnote n="17">17 JOHN 21 derive limits on leptophilic DM annihilating to positrons by comparing expected spectra to AMS-02 data. The range m(DM): 60-300 GeV appears excluded for this type of model, see Fig. 3.</footnote>

<footnote n="18">18 ABDAZAJIAN 20 derive new limits on WIMP annihilation in galactic center (GC): $\langle\sigma\cdot\nu\rangle < 2.5 \times 10^{-27}$ cm$^3$/s for m(WIMP) = 50 GeV; seems to rule out WIMP explanation for GC γ excess, favouring an astrophysics origin.</footnote>

<footnote n="19">19 ABDALLAH 20 search for WIMP annihilation in newly discovered by DES dwarf satellite galaxies using HESS; limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(DM) plane depending on annihilation channel and which dwarf satellite.</footnote>

<footnote n="20">20 ABE 20G search Super-famiokande data for WIMP annihilation to neutrinos in galactic center/halo; no signal; limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(DM) plane depending on annihilation channel and m(WIMP). Reported limit for annihilation to $\nu\bar{\nu}$ at 1 GeV.</footnote>

<footnote n="21">21 ALBERT 20 search for TeV-scale WIMP annihilation to γγ in dwarf spheroidal galaxies; no signal; limits placed in $\sigma\cdot\nu$ vs m(WIMP) plane: e.g. $\sigma\cdot\nu < 2.2 \times 10^{-24}$ cm$^3$/s for m(WIMP) = 1 TeV.</footnote>

<footnote n="22">22 ALBERT 20A search for WIMP annihilation to νs in galactic center using Antares; limits placed in $\sigma\cdot\nu$ vs m(WIMP) plane e.g. $\sigma\cdot\nu < 5 \times 10^{-24}$ cm$^3$/s for m(WIMP) = 1 TeV assuming annihilation dominantly to $\tau\bar{\tau}$.</footnote>

<footnote n="23">23 ALBERT 20C report combined Antares + IceCube search for WIMP annihilation to $\tau\bar{\tau}$; for NFW halo profile report $\sigma\cdot\nu < 1 \times 10^{-23}$ cm$^3$/s for m(WIMP) = 100 GeV.</footnote>

<footnote n="24">24 ALVAREZ 20 use profiling over J-factor distributions and background to derive new limits on $\sigma\cdot\nu$; e.g. $\sigma\cdot\nu < 8 \times 10^{-26}$ cm$^3$/s for m(WIMP) = 100 GeV.</footnote>

<footnote n="25">25 HOOF 20 examine γ rays from 27 dwarf spheroids using Fermi-LAT data; place limits in $\sigma\cdot\nu$ vs m(WIMP) plane using profile likelihood and marginalized posterior techniques for DM annihilation to $\tau\bar{\tau}$ and b$\bar{b}$; quoted limit uses first technique and b$\bar{b}$ channel for m(WIMP) = 100 GeV; results rule out WIMP explanation of galactic center excess.</footnote>

<footnote n="26">26 MAZZIOTTA 20 use Fermi-LAT pointed-at-Sun data to search for DM annihilation in the Sun to long-lived mediators decaying into gamma rays, i.e. $\chi\chi \to \phi\phi \to 4\gamma$. Limits placed on the SI and SD DM-nucleon cross sections in the $\alpha$-DM mass plane for DM masses in the range 3 GeV - 1.8 TeV. Limits are evaluated in both cases of equilibrium and non-equilibrium.</footnote>

<footnote n="27">27 ABEYSEKARA 19 search for γs from DM annihilation in galactic substructures with HAWC; no signal, limits placed in $J\langle\sigma\cdot\nu\rangle$ vs. declination plane for m(DM) ~ 1-108 TeV.</footnote>

<footnote n="28">28 ALBERT 19B search for DM signal from M31 galaxy in μ, τ, t, b, W channels using HAWC for m(DM) ~ 1-100 TeV; no signal, limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(DM) plane.</footnote>

<footnote n="29">29 CHEUNG 19 derive model-dependent bounds on $\langle\sigma\cdot\nu\rangle$ from EDGES data: $< 4 \times 10^{-26}$ cm$^3$/s for $e^+e^-$ and b$\bar{b}$ for m(χ) = 100 GeV (including boost factor).</footnote>

<footnote n="30">30 DI-MAURO 19 place limits on WIMP annihilation via Fermi-LAT observation of M31 and M33 galaxies: $\langle\sigma\cdot\nu\rangle < 7 \times 10^{-27}$ cm$^3$/s for m(χ) = 20 GeV from M31.</footnote>

<footnote n="31">31 JOHNSON 19 search for γ-rays, 10-600 GeV energy, from P-wave annihilating DM around SgrA* BH using Fermi-LAT; limits set for various models.</footnote>

<footnote n="32">32 LI 19D search for $\chi\chi \to \gamma$ in Fermi-LAT data; no signal, require $\langle\sigma\cdot\nu\rangle < 2 \times 10^{-26}$ cm$^3$/s for m(χ) = 100 GeV.</footnote>

<footnote n="33">33 NG 19 search for X-ray line from sterile ν decay/annihilation using NuStar M-31; no signal: limits placed in m(ν) vs mixing angle and $\langle\sigma\cdot\nu\rangle$ vs m(ν).</footnote>

<footnote n="34">34 QUEIROZ 19 examine $\chi\chi \to \chi SM$ semi-annihilation of DM reaction; limits placed for various assumed SM particles in $\langle\sigma\cdot\nu\rangle$ vs. m(χ) plane.</footnote>

<footnote n="35">35 ABDALLAH 18 search for WIMP WIMP → γX in central galactic halo, 10 years of data; limits placed in $\langle\sigma\cdot\nu\rangle$ vs. m(WIMP) plane for m(WIMP): 0.3-70 TeV.</footnote>
36 AHNEN 18 search for WIMP WIMP → γX from Ursa Major II; limits set in $\langle\sigma\cdot\nu\rangle$ vs. m(WIMP) plane for $b\bar{b}$, $W^+W^-$, $\tau^+\tau^-$, and $\mu^+\mu^-$ annihilation modes.

37 ALBERT 18B search for TeV-scale WIMPs with WIMP WIMP → γX in Andromeda galaxy using HAWC Observatory; limits set in $\langle\sigma\cdot\nu\rangle$ vs m(WIMP) plane.

38 CHANG 18A examine $\chi\chi \to b\bar{b} \to \gamma$ using Fermi Pass 8 data; no signal; require $\langle\sigma\cdot\nu\rangle < 10^{-26} \text{ cm}^3/\text{s}$ for m(χ) = 50 MeV.

39 LISANTI 18 examine Fermi Pass 8 γ-ray data from galaxy groups; report m(WIMP) > 30 GeV for annihilation in $b\bar{b}$ channel.

40 MAZZIOTTA 18 examine Fermi-LAT electron and positron spectra searching for features originating from DM particles annihilation into $e^+e^-$ pairs, from 45 GeV to 2 TeV; no signal found, limits are obtained.

41 AARTSEN 17C use 1005 days of IceCube data to search for $\chi\chi \to$ neutrinos via various annihilation channels. Limits set.

42 ALBERT 17A search for DM annihilation to $\nu s$ using ANTARES data from 2007–2015. No signal. Limits set in $\langle\sigma\cdot\nu\rangle$ vs. m(DM) plane for m(DM) ~10–10×10⁵ GeV. The listed limit is for m(DM) = 100 TeV.

43 ARCHAMBULT 17 set limits for WIMP mass between 100 GeV and 1 TeV on $\langle\sigma\cdot\nu\rangle$ for $W^+W^-$, $ZZ$, $b\bar{b}$, $s\bar{s}$, $u\bar{u}$, $d\bar{d}$, $t\bar{t}$, $e^+e^-$, $gg$, $c\bar{c}$, $hh$, $\gamma\gamma$, $\mu^+\mu^-$, $\tau^+\tau^-$ annihilation channels.

44 AVRIN 17 find upper limits for the annihilation cross section in various channels for DM particle mass between 30 GeV and 10 TeV. Strongest upper limits coming from the two neutrino channel require $\langle\sigma\cdot\nu\rangle < 6 \times 10^{-20} \text{ cm}^3/\text{s}$ in dwarf galaxies and $\langle\sigma\cdot\nu\rangle < 7 \times 10^{-21} \text{ cm}^3/\text{s}$ in LMC for 5 TeV WIMP mass.

45 BOUDAUD 17 use data from the spacecraft Voyager 1, beyond the heliopause, and from AMS02 on $\chi\chi \to e^+e^-$ to require $\langle\sigma\cdot\nu\rangle < 1 \times 10^{-28} \text{ cm}^3/\text{s}$ for m(χ) = 10 MeV.

46 AARTSEN 16D search for $\nu\nu$ vs from WIMP annihilation in galaxy; limits set on $\langle\sigma\cdot\nu\rangle$ in Fig. 6, 7.

47 ABDALLAH 16 require $\langle\sigma\cdot\nu\rangle < 6 \times 10^{-26} \text{ cm}^3/\text{s}$ for m(WIMP) = 1.5 TeV from 254 hours observation (WW channel) and < 2 × 10$^{-26}$ cm$^3/\text{s}$ for m(WIMP) = 1.0 TeV in $\tau^+\tau^-$ channel.

48 ABDALLAH 16A search for line spectra from WIMP + WIMP → γγ in 18 hr HESS data; rule out previous 130 GeV WIMP hint from Fermi-LAT data.

49 AHNEN 16 require $\langle\sigma\cdot\nu\rangle < 3 \times 10^{-26} \text{ cm}^3/\text{s}$ for m(WIMP) = 100 GeV (WW channel).

50 AVRIN 16 require $\langle\nu\nu\rangle < 1.91 \times 10^{-21} \text{ cm}^3/\text{s}$ from WIMP annihilation to $\nu s$ via WW channel for m(WIMP) = 1 TeV.

51 CAPUTO 16 place limits on WIMPs from annihilation to gamma rays in Small Magellanic Cloud using Fermi-LaT data: $\langle\sigma\cdot\nu\rangle < 3 \times 10^{-26} \text{ cm}^3/\text{s}$ for m(WIMP) = 10 GeV.

52 FORNASA 16 use anisotropies in the γ-ray diffuse emission detected by Fermi-LAT to bound $\langle\sigma\cdot\nu\rangle < 10^{-25} \text{ cm}^3/\text{s}$ for m(WIMP) = 100 GeV in $b\bar{b}$ channel: see Fig. 28. The limit is driven by dark-matter subhalos in the Milky Way and it refers to their Most Constraining Scenario.

53 LEITE 16 constrain WIMP annihilation via search for radio emissions from Smith cloud; $\langle\sigma\cdot\nu\rangle < 5 \times 10^{-27} \text{ cm}^3/\text{s}$ in e e channel for m(WIMP) = 5 GeV.

54 LI 16 re-analyze Fermi-LAT data on 8 dwarf spheroidals; set limit $\langle\sigma\cdot\nu\rangle < 2 \times 10^{-26} \text{ cm}^3/\text{s}$ for m(WIMP) = 100 GeV in $b\bar{b}$ mode with substructures included.

55 LI 16A constrain $\langle\sigma\cdot\nu\rangle < 10^{-25} \text{ cm}^3/\text{s}$ in $b\bar{b}$ channel for m(WIMP) = 100 GeV using Fermi-LAT data from M31; see Fig. 6.

56 LIANG 16 search dwarf spheroidal galaxies, Large Magellanic Cloud, and Small Magellanic Cloud for γ-line in Fermi-LAT data.

57 LU 16 re-analyze Fermi-LAT and AMS-02 data; require $\langle\sigma\cdot\nu\rangle < 10^{-25} \text{ cm}^3/\text{s}$ for $m_t$ (WIMP) = 1 TeV in $b\bar{b}$ channel.

58 SHIRASAKI 16 re-anayze Fermi-LAT extra-galactic data; require $\langle\sigma\cdot\nu\rangle < 10^{-23} \text{ cm}^3/\text{s}$ for m(WIMP) = 1 TeV in $b\bar{b}$ channel; see Fig. 8.

59 AARTSEN 15C search for neutrinos from $\chi^0$ annihilation in the Galactic halo. See their Figs. 16 and 17, and Table 5 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 100 GeV and 100 TeV.

60 AARTSEN 15E search for neutrinos from $\chi^0$ annihilation in the Galactic center. See their Figs. 7 and 9, and Table 3 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 30 GeV and 10 TeV.

61 ABRAMOWSKI 15 search for γ from $\chi^0$ annihilation in the Galactic center. See their Fig. 4 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 250 GeV and 10 TeV.

62 ACKERMANN 15 search for monochromatic γ from $\chi^0$ annihilation in the Galactic halo. See their Fig. 8 and Tables 2–4 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 0.2 GeV and 500 GeV.

63 ACKERMANN 15a search for γ from $\chi^0$ annihilation (both Galactic and extragalactic) in the isotropic γ background. See their Fig. 7 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 10 GeV and 30 TeV.

64 ACKERMANN 15b search for γ from $\chi^0$ annihilation in 15 dwarf spheroidal satellite galaxies of the Milky Way. See their Figs. 1 and 2 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 2 GeV and 10 TeV.

65 ADRIAN-MARTINEZ 15 search for neutrinos from $\chi^0$ annihilation in the Galactic center. See their Figs. 10 and 11 and Tables 1 and 2 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 25 GeV and 10 TeV.

66 ACKERMANN 14 search for γ from $\chi^0$ annihilation in 25 dwarf spheroidal satellite galaxies of the Milky Way. See their Tables II-VII for limits assuming annihilation into $e^+e^-$, $\mu^+\mu^-$, $\tau^+\tau^-$, $u\bar{u}$, $b\bar{b}$, and $W^+W^-$, for $\chi^0$ mass ranging from 2 GeV to 10 TeV.

67 Limit assuming $\chi^0$ pair annihilation into $b\bar{b}$.

68 Limit assuming $\chi^0$ pair annihilation into $W^+W^-$.

69 ALEKSIC 14 search for γ from $\chi^0$ annihilation in the dwarf spheroidal galaxy Segue 1. The listed limit assumes annihilation into $W^+W^-$, See their Figs. 6, 7, and 16 for limits on $\sigma\cdot\nu$ for annihilation channels $\mu^+\mu^-$, $\tau^+\tau^-$, $b\bar{b}$, $t\bar{t}$, $\gamma\gamma$, $\gamma Z$, $W^+W^-$, $ZZ$ for $\chi^0$ mass between 10² and 10⁴ GeV.

70 AARTSEN 13 search for neutrinos from $\chi^0$ annihilation in nearby galaxies and galaxy clusters. See their Figs. 5–7 for limits on $\sigma\cdot\nu$ for $\chi^0\chi^0 \to \nu\bar{\nu}$, $\mu^+\mu^-$, $\tau^+\tau^-$, and $W^+W^-$ for $\chi^0$ mass between 300 GeV and 100 TeV.

71 ABRAMOWSKI 13 search for monochromatic γ from $\chi^0$ annihilation in the Milky Way halo in the central region. Limit on $\sigma\cdot\nu$ between $10^{-28}$ and $10^{-25} \text{ cm}^3 \text{s}^{-1}$ (95% CL) is obtained for $\chi^0$ mass between 500 GeV and 20 TeV for $\chi^0\chi^0 \to \gamma\gamma$. $\chi^0$ density distribution in the Galaxy by Einasto is assumed. See their Fig. 4.

72 ACKERMANN 13A search for monochromatic γ from $\chi^0$ annihilation in the Milky Way. Limit on $\sigma\cdot\nu$ for the process $\chi^0\chi^0 \to \gamma\gamma$ in the range $10^{-29}-10^{-27} \text{ cm}^3 \text{s}^{-1}$ (95% CL) is obtained for $\chi^0$ mass between 5 and 300 GeV. The limit depends slightly on the assumed density profile of $\chi^0$ in the Galaxy. See their Tables VII–X and Fig. 10. Supersedes ACKERMANN 12.

73 ABRAMOWSKI 12 search for γ's from $\chi^0$ annihilation in the Fornax galaxy cluster. See their Fig. 7 for limits on $\sigma\cdot\nu$ for $\chi^0$ mass between 0.1 and 100 TeV for the annihilation channels $\tau^+\tau^-$, $b\bar{b}$, and $W^+W^-$.

74 ACKERMANN 12 search for monochromatic γ from $\chi^0$ annihilation in the Milky Way. Limit on $\sigma\cdot\nu$ in the range $10^{-28}-10^{-26} \text{ cm}^3 \text{s}^{-1}$ (95% CL) is obtained for $\chi^0$ mass between 7 and 200 GeV if $\chi^0$ annihilates into $\gamma\gamma$. The limit depends slightly on the assumed density profile of $\chi^0$ in the Galaxy. See their Table III and Fig. 15.

75 ACKERMANN 12 search for γ from $\chi^0$ annihilation in the Milky Way in the diffuse γ background. Limit on $\sigma\cdot\nu$ of $10^{-24} \text{ cm}^3 \text{s}^{-1}$ or larger is obtained for $\chi^0$ mass between 5 GeV and 10 TeV for various annihilation channels including $W^+W^-$, $b\bar{b}$, $gg$, $e^+e^-$, $\mu^+\mu^-$, $\tau^+\tau^-$, $b\bar{b}$, and $W^+W^-$. See their Figs. 17–20.

76 ALIU 12 search for γ's from $\chi^0$ annihilation in the dwarf spheroidal galaxy Segue 1. Limit on $\sigma\cdot\nu$ in the range $10^{-24}-10^{-20} \text{ cm}^3 \text{s}^{-1}$ (95% CL) is obtained for $\chi^0$ mass between 10 GeV and 2 TeV for annihilation channels $e^+e^-$, $\mu^+\mu^-$, $\tau^+\tau^-$, $b\bar{b}$, and $W^+W^-$. See their Fig. 3.

77 BASBARI 11C search for $\nu_\mu$ from $\chi^0$ annihilation in the outer halo of the Milky Way. The limit assumes annihilation into $\nu\nu$. See their Fig. 9 for limits with other annihilation channels.

78 ABRAMOWSKI 11 search for γ from $\chi^0$ annihilation near the Galactic center. The limit assumes Einasto DM density profile.

79 ACKERMANN 11 search for γ from $\chi^0$ annihilation in ten dwarf spheroidal satellite galaxies of the Milky Way. The limit for m = 10 GeV assumes annihilation into $b\bar{b}$, the others $W^+W^-$, See their Fig. 2 for limits with other final states. See also GERINGER-SAMETH 11 for a different analysis of the same data.

## Dark Matter Particle ($\chi^0$) Production in Hadron Collisions

Searches for $\chi^0$ production in association with observable particles (γ, jets, ...) in high energy hadron collisions. If a specific form of effective interaction Lagrangian is assumed, the limits may be translated into limits on $\chi^0$-nucleon scattering cross section.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td>We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1</td><td>AAD</td><td>23A ATLS</td><td>H → invisible search</td></tr><tr><td>2</td><td>AAD</td><td>23AF ATLS</td><td>t̄t + H → invisible search</td></tr><tr><td>3</td><td>AAD</td><td>23AJ ATLS</td><td>extended 2HDM search</td></tr><tr><td>4</td><td>AAD</td><td>23BX ATLS</td><td>H<sub>a</sub>, a → DM search</td></tr><tr><td>5</td><td>AAD</td><td>23W ATLS</td><td>dark Higgs model</td></tr><tr><td>6</td><td>AKIMOV</td><td>23 COHR</td><td>LDM search at SNS</td></tr><tr><td>7</td><td>LIN</td><td>23C KOTO</td><td>χ → γγ from K<sub>L</sub><sup>0</sup> decay</td></tr><tr><td>8</td><td>AAD</td><td>22D ATLS</td><td>Z<sup>+</sup>H with H → DM</td></tr><tr><td>9</td><td>AAD</td><td>22P ATLS</td><td>H → χχ search via VBF</td></tr><tr><td>10</td><td>AGUILAR-AR...</td><td>22A CCM</td><td>p dump search for MeV-scale DM</td></tr><tr><td>11</td><td>TUMASYAN</td><td>22AA CMS</td><td>Z<sup>+</sup> → DM search</td></tr><tr><td>12</td><td>TUMASYAN</td><td>22AG CMS</td><td>strongly interacting DM search</td></tr><tr><td>13</td><td>TUMASYAN</td><td>22G CMS</td><td>DM search via VBF to Higgs</td></tr><tr><td>14</td><td>AAD</td><td>21AZ ATLS</td><td>DM search in H E<sub>T</sub> → γγ E<sub>T</sub></td></tr><tr><td>15</td><td>AAD</td><td>21BB ATLS</td><td>DM search in H E<sub>T</sub> → b<span style="text-decoration: overline">b</span> E<sub>T</sub></td></tr><tr><td>16</td><td>AAD</td><td>21D ATLS</td><td>Dark Higgs</td></tr><tr><td>17</td><td>AAD</td><td>21F ATLS</td><td>jet + missing momentum</td></tr><tr><td>18</td><td>AAD</td><td>21K ATLS</td><td>photon + DM</td></tr><tr><td>19</td><td>AAD</td><td>21O ATLS</td><td>ℓ + jets + E<sub>T</sub> to search for t-pairs + DM</td></tr><tr><td>20</td><td>AAD</td><td>21P ATLS</td><td>ℓ<sup>+</sup>ℓ<sup>+</sup> + jets + E<sub>T</sub></td></tr><tr><td>21</td><td>AAD</td><td>21S ATLS</td><td>b-jets + E<sub>T</sub></td></tr><tr><td>22</td><td>SIRUNYAN</td><td>21A CMS</td><td>pp → Zχχ; Z → t<span style="text-decoration: overline">t</span></td></tr><tr><td>23</td><td>SIRUNYAN</td><td>21D ATLS</td><td>DM search in jets + E<sub>T</sub></td></tr><tr><td>24</td><td>SIRUNYAN</td><td>20X CMS</td><td>pp → Z<sup>+</sup> → A(Z<sup>+</sup>)h → h + E<sub>T</sub></td></tr><tr><td>25</td><td>AABOUD</td><td>19AA ATLS</td><td>multi-channel BSM search</td></tr><tr><td>26</td><td>AABOUD</td><td>19AI ATLS</td><td>H → χχ</td></tr><tr><td>27</td><td>AABOUD</td><td>19AL ATLS</td><td>H → χχ</td></tr><tr><td>28</td><td>AABOUD</td><td>19O ATLS</td><td>single t + E<sub>T</sub></td></tr><tr><td>29</td><td>AABOUD</td><td>19V ATLS</td><td>review mediator based DM searches</td></tr><tr><td>30</td><td>BANERJEE</td><td>19 NA64</td><td>eN → eN + E<sub>T</sub></td></tr><tr><td>31</td><td>SIRUNYAN</td><td>19AN CMS</td><td>Hχχ → b<span style="text-decoration: overline">b</span> E<sub>T</sub></td></tr><tr><td>32</td><td>SIRUNYAN</td><td>19BC CMS</td><td>LQ LQ → µj E<sub>T</sub></td></tr><tr><td>33</td><td>SIRUNYAN</td><td>19BO CMS</td><td>VV → Hqq; H → DM</td></tr><tr><td>34</td><td>SIRUNYAN</td><td>19C CMS</td><td>pp → t<span style="text-decoration: overline">t</span>χχ</td></tr><tr><td>35</td><td>SIRUNYAN</td><td>19O CMS</td><td>pp → γ E<sub>T</sub></td></tr><tr><td>36</td><td>SIRUNYAN</td><td>19X CMS</td><td>pp → t<span style="text-decoration: overline">t</span> + ν̄t; pp → t<span style="text-decoration: overline">t</span> + ν̄t</td></tr><tr><td>37</td><td>AABOUD</td><td>18 ATLS</td><td>pp → Zχχ; Z → ℓℓ</td></tr><tr><td>38</td><td>AABOUD</td><td>18A ATLS</td><td>pp → t<span style="text-decoration: overline">t</span> E<sub>T</sub>; pp → b<span style="text-decoration: overline">b</span> E<sub>T</sub></td></tr><tr><td>39</td><td>AABOUD</td><td>18CA ATLS</td><td>pp → Vχχ; V → jj</td></tr><tr><td>40</td><td>AABOUD</td><td>18I ATLS</td><td>pp → jet(s) + E<sub>T</sub></td></tr><tr><td>41</td><td>AABOUD</td><td>18B ATLS</td><td>pp → Z<span style="text-decoration: overline">Z</span> + E<sub>T</sub></td></tr><tr><td>42</td><td>SIRUNYAN</td><td>18BF CMS</td><td>pp → t E<sub>T</sub></td></tr><tr><td>43</td><td>SIRUNYAN</td><td>18BO CMS</td><td>dijet resonance search</td></tr><tr><td>44</td><td>SIRUNYAN</td><td>18BV CMS</td><td>pp → Z E<sub>T</sub></td></tr><tr><td>45</td><td>SIRUNYAN</td><td>18C CMS</td><td>pp → t<span style="text-decoration: overline">t</span> E<sub>T</sub></td></tr><tr><td>46</td><td>SIRUNYAN</td><td>18C CMS</td><td>pp → t<span style="text-decoration: overline">t</span> E<sub>T</sub></td></tr></tbody></table>
<table>
  <tbody>
    <tr>
      <td>47</td>
      <td>SIRUNYAN</td>
      <td>18CU</td>
      <td>CMS</td>
      <td>pp &rarr; Z &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>48</td>
      <td>SIRUNYAN</td>
      <td>18DH</td>
      <td>CMS</td>
      <td>pp &rarr; &chi;&chi;h; h &rarr; &gamma;&gamma; or &tau;&tau;</td>
    </tr>
    <tr>
      <td>49</td>
      <td>SIRUNYAN</td>
      <td>18S</td>
      <td>CMS</td>
      <td>pp &rarr; jets &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>50</td>
      <td>AABOUD</td>
      <td>17A</td>
      <td>ATLS</td>
      <td>pp (H &rarr; b&delta; + WIMP pair)</td>
    </tr>
    <tr>
      <td>51</td>
      <td>AABOUD</td>
      <td>17AM</td>
      <td>ATLS</td>
      <td>pp &rarr; Z' &rarr; Ah &rarr; h(b&delta;) + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>52</td>
      <td>AABOUD</td>
      <td>17AQ</td>
      <td>ATLS</td>
      <td>pp &rarr; h(&gamma;&gamma;) + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>53</td>
      <td>AABOUD</td>
      <td>17BD</td>
      <td>ATLS</td>
      <td>pp &rarr; jet(s) + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>54</td>
      <td>AABOUD</td>
      <td>17R</td>
      <td>ATLS</td>
      <td>pp &rarr; &gamma;E<sub>T</sub></td>
    </tr>
    <tr>
      <td>55</td>
      <td>AGUILAR-AR...</td>
      <td>17A</td>
      <td>MBNE</td>
      <td>pN &rarr; &chi;&chi;X; &chi;N &rarr; &chi;N</td>
    </tr>
    <tr>
      <td>56</td>
      <td>BANERJEE</td>
      <td>17</td>
      <td>NA64</td>
      <td>eN &rarr; eN&gamma;</td>
    </tr>
    <tr>
      <td>57</td>
      <td>KHACHATRY...</td>
      <td>17A</td>
      <td>CMS</td>
      <td>forward jets + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>58</td>
      <td>KHACHATRY...</td>
      <td>17F</td>
      <td>CMS</td>
      <td>H &rarr; invisibles</td>
    </tr>
    <tr>
      <td>59</td>
      <td>SIRUNYAN</td>
      <td>17</td>
      <td>CMS</td>
      <td>Z + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>60</td>
      <td>SIRUNYAN</td>
      <td>17AP</td>
      <td>CMS</td>
      <td>pp &rarr; Z' &rarr; Ah &rarr; h + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>61</td>
      <td>SIRUNYAN</td>
      <td>17AQ</td>
      <td>CMS</td>
      <td>pp &rarr; &gamma; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>62</td>
      <td>SIRUNYAN</td>
      <td>17BB</td>
      <td>CMS</td>
      <td>pp &rarr; t&tau; + &epsilon;<sub>T</sub>; pp &rarr; b&delta; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>63</td>
      <td>SIRUNYAN</td>
      <td>17G</td>
      <td>CMS</td>
      <td>pp &rarr; j + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>64</td>
      <td>SIRUNYAN</td>
      <td>17U</td>
      <td>CMS</td>
      <td>pp &rarr; Z&chi;&chi;; Z &rarr; &ell;&ell;</td>
    </tr>
    <tr>
      <td>65</td>
      <td>AABOUD</td>
      <td>16AD</td>
      <td>ATLS</td>
      <td>(W or Z &rarr; jets) + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>66</td>
      <td>AAD</td>
      <td>16AF</td>
      <td>ATLS</td>
      <td>VV &rarr; forward jets + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>67</td>
      <td>AAD</td>
      <td>16AG</td>
      <td>ATLS</td>
      <td>&ell; + jets</td>
    </tr>
    <tr>
      <td>68</td>
      <td>AAD</td>
      <td>16M</td>
      <td>ATLS</td>
      <td>pp &rarr; H + &epsilon;<sub>T</sub>, H &rarr; b&delta;</td>
    </tr>
    <tr>
      <td>69</td>
      <td>KHACHATRY...</td>
      <td>16BZ</td>
      <td>CMS</td>
      <td>jet(s) + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>70</td>
      <td>KHACHATRY...</td>
      <td>16CA</td>
      <td>CMS</td>
      <td>jets + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>71</td>
      <td>KHACHATRY...</td>
      <td>16N</td>
      <td>CMS</td>
      <td>pp &rarr; &gamma; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>72</td>
      <td>AAD</td>
      <td>15AS</td>
      <td>ATLS</td>
      <td>b(&delta;) + &epsilon;<sub>T</sub>, t&tau; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>73</td>
      <td>AAD</td>
      <td>15BH</td>
      <td>ATLS</td>
      <td>jet + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>74</td>
      <td>AAD</td>
      <td>15CF</td>
      <td>ATLS</td>
      <td>H<sup>0</sup> + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>75</td>
      <td>AAD</td>
      <td>15CS</td>
      <td>ATLS</td>
      <td>&gamma; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>76</td>
      <td>KHACHATRY...</td>
      <td>15AG</td>
      <td>CMS</td>
      <td>t&tau; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>77</td>
      <td>KHACHATRY...</td>
      <td>15AL</td>
      <td>CMS</td>
      <td>jet + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>78</td>
      <td>KHACHATRY...</td>
      <td>15T</td>
      <td>CMS</td>
      <td>&ell; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>79</td>
      <td>AAD</td>
      <td>14AI</td>
      <td>ATLS</td>
      <td>W + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>80</td>
      <td>AAD</td>
      <td>14BK</td>
      <td>ATLS</td>
      <td>W, Z + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>81</td>
      <td>AAD</td>
      <td>14K</td>
      <td>ATLS</td>
      <td>Z + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>82</td>
      <td>AAD</td>
      <td>14O</td>
      <td>ATLS</td>
      <td>Z + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>83</td>
      <td>AAD</td>
      <td>13AD</td>
      <td>ATLS</td>
      <td>jet + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>84</td>
      <td>AAD</td>
      <td>13C</td>
      <td>ATLS</td>
      <td>&gamma; + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>85</td>
      <td>AALTONEN</td>
      <td>12K</td>
      <td>CDF</td>
      <td>t + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>86</td>
      <td>AALTONEN</td>
      <td>12M</td>
      <td>CDF</td>
      <td>jet + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>87</td>
      <td>CHATRCHYAN...</td>
      <td>12AP</td>
      <td>CMS</td>
      <td>jet + &epsilon;<sub>T</sub></td>
    </tr>
    <tr>
      <td>88</td>
      <td>CHATRCHYAN...</td>
      <td>12T</td>
      <td>CMS</td>
      <td>&gamma; + &epsilon;<sub>T</sub></td>
    </tr>
  </tbody>
</table>

1 AAD 23A search for $H \to$ invisible. No signal observed. Results interpreted in terms of several DM Higgs portal simplified models.

2 AAD 23A search for $t\bar{t} + H \to$ invisible with 139 fb⁻¹ of data. No signal observed. Limits placed on branching fractions of H decays etc. for various DM mediator models. Result also included in AAD 23A.

3 AAD 23A search for $tW\chi\chi$ production in mediator-extended 2HDM with 139 fb⁻¹ of data. No signal observed. Limits placed in m(H) vs. m(mediator) and tan(β) vs. m(H) planes.

4 AAD 23B search for $A \to H\bar{a}$ production where $H \to \tau\bar{\tau}$ and $a \to \chi\chi$. No signal observed. Limits placed on 2HDM+a model.

5 AAD 23W search for DM in dark Higgs model via WW$\chi\chi$ final state with 139 fb⁻¹ of data. No signal detected. Limits set in m(m dark Higgs) vs. m(Z') plane.

6 AKIMOV 23 search for light DM via COHERENT Csl detector at SNS. No signal observed. For scalar DM model, limits set for m(χ) = 1–300 MeV. Limit of σ(χN) < 1 × 10¹¹ pb set at peak sensitivity m(χ) = 25 MeV.

7 LIN 23C search for $\chi \to \gamma\gamma$ decay where $p \to \chi\chi$ at KOTO. No signal observed. Limits placed on $K_L^0$ branching fraction.

8 AAD 22D search for $Z+H$ production with $Z \to t\bar{t}$ and $H \to \chi\chi$ with 139 fb⁻¹ at 13 TeV; no signal found; limits placed in various simplified models depending on Higgs portal and DM mediator.

9 AAD 22P search for $H$ production via VBF with $H \to \chi\chi$ with 139 fb⁻¹ at 13 TeV; no signal found; limits placed for various Higgs DM portal simplified models.

10 AGUILAR-AREVALO 22A report search for MeV vector portal and leptophobic DM via scatter on liquid Ar at the Lujan stopped pion source at LANL; no signal detected; limits placed on vector portal and leptophobic DM vs. m(χ): 1–40 MeV.

11 TUMASYAN 22AA search for $Z'$ decay to dark quarks with 138 fb⁻¹ at 13 TeV; no signal observed; limits exclude a wide range of strongly coupled hidden sector models.

12 TUMASYAN 22AG search for strongly interacting dark matter production via scalar mediator, with SIMP decay to trackless jets with 16.1 fb⁻¹ at 13 TeV; no signal detected; limits placed in mass vs. cross section plane for simplified models.

13 TUMASYAN 22c search for VBF production of Higgs with $H \to \chi\chi$ with 101 fb⁻¹ at 13 TeV, combined with earlier searches, in total 19.7 fb⁻¹ at 8 TeV and 140 fb⁻¹ at 13 TeV are used; no signal detected; limits placed in mass vs. cross section plane for various Higgs portal simplified models.

14 AAD 21AZ search for DM in $H \to \bar{E}_T \to \gamma\gamma E_T$ events with 139 fb⁻¹ at 13 TeV. No signal observed. Limits placed for several simplified models.

15 AAD 21BB search for DM in $H \to \bar{E}_T \to b\bar{b} E_T$ events with 139 fb⁻¹ at 13 TeV. No signal observed. Limits placed for several simplified models.

16 AAD 21D search for $VV + \chi\chi, V \to q\bar{q}$ with 139 fb⁻¹ at 13 TeV LHC. No signal detected. Limits placed in dark Higgs boson mass vs. m(Z') plane. Here VV stand for $W \pm W \mp Z, Z$.

17 AAD 21f search for monojet recoiling against invisibles with 139 fb⁻¹ at 13 TeV LHC. No signal detected. Limits placed in various simplified dark matter models.

18 AAD 21k search for a photon recoiling against dark matter with 139 fb⁻¹ at 13 TeV LHC. No signal detected. Limits placed on parameter space of various simplified models.

19 AAD 21D search for $\ell + jets + E_T$ to search for $t$-pairs + DM particles with 139 fb⁻¹ at LHC 13 TeV LHC. No signal detected. Limits placed in the cross-section vs. mediator mass plane, assuming light DM states.

20 AAD 21P search for $\ell^+\ell^- + jets + E_T$ in context of various BSM models with 139 fb⁻¹ at 13 TeV LHC. No signal observed. Limits placed in parameter space of dark matter models and SUSY.

21 AAD 21S search for $b$-jets + $E_T$ signal from BSM/DM models with 139 fb⁻¹ at 13 TeV LHC. No signal observed. Limits placed on parameter space of DM models.

22 SIRUNYAN 21A search for DM production in association with leptonically decaying Z boson in 137 fb⁻¹ at 13 TeV; no signal; limits set in large variety of simplified DM models.

23 TUMASYAN 21D search for DM and other exotic at CMS in jets + $\bar{E}_T$ events with 137 fb⁻¹ at 13 TeV. No signal observed. Limits placed for a variety of simplified models.

24 SIRUNYAN 20x search for DM in $pp \to Z' \to A(Z')h \to h + E_T$ in CMS at 13 TeV with 35.9 fb⁻¹; no signal; limits placed in $\sigma^{\text{ST}}$ vs. m(χ), and $\sigma$, m(A) and $\tan\beta$ vs m(Z') for considered DM models.

25 AABOUD 19AA searches for BSM physics in more than 700 event classes with more than 10⁵ regions at 13 TeV with 3.2 fb⁻¹; no significant signal.

26 AABOUD 19AI search for vector boson fusion $pp \to Hqq, H \to$ invisible at 13 TeV with 36.1 fb⁻¹; no signal: require $B(H \to$ invisible) < 0.37 (0.28 expected).

27 AABOUD 19AL perform search in three different channels for $H \to \chi\chi$ at 7, 8 and 13 TeV; combined result BF($H \to$ invisible) < 0.26 (0.17 expected).

28 AABOUD 19Q search for single $t + E_T$ at 13 TeV with 36.1 fb⁻¹ of data; no signal; limits set in $\sigma$ or coupling vs. mass plane for simplified models.

29 AABOUD 19V review ATLAS results from 7, 8 and 13 TeV searches for mediator-based DM and DE scalar which couples to gravity; no signal; limits set for large variety of simplified models.

30 BANERJEE 19 search for dark photon via $eN \to eN+\bar{E}$ in NA64; no signal, limits placed in kinetic mixing $\epsilon$ vs. m(DM) plane for m(DM) ~ 0.001–1 GeV.

31 SIRUNYAN 19AN search at 13 TeV with 35.9 fb⁻¹ for $pp \to H\chi\chi \to b\bar{b} E_T$; no signal: limits set in the context of a 2HDM + pseudoscalar (a) model and a baryonic $Z'$ model.

32 SIRUNYAN 19BC search for DM via LeptoQuark pair annihilation LQ LQ → $\mu j \chi \chi \to \mu j E_T$ with 77.4 fb⁻¹, 13 TeV; no signal: limits placed in m(χ) vs. m(LQ) plane. Model dependent limits on DM mass up to 600 GeV placed on m(LQ) placed.

33 SIRUNYAN 19B0 search for vector boson fusion $VV \to q\bar{q}H$ with $H \to \chi\chi$ at 13 TeV with 38.2 fb⁻¹; no signal: limits placed for several models. Also search for $H \to$ invisible at 7, 8, and 13 TeV; no signal: limit placed on BF < 0.19.

34 SIRUNYAN 19C search for DM via $pp \to t\bar{t}\chi\chi$ at 13 TeV, 35.9 fb⁻¹; no signal; limits placed on coupling vs. mediator mass for various simplified models.

35 SIRUNYAN 19D search for $pp \to \gamma$ at 13 TeV with 35.9 fb⁻¹; no signal: limits placed on parameters of various models.

36 SIRUNYAN 19x search for $pp \to t\bar{t} E_T$ and $pp \to t E_T + ...$ at 13 TeV with 35.9 fb⁻¹; no signal: limits placed on $\chi$ production $\sigma$ for various simplified models with m(χ) = 1 GeV.

37 AABOUD 18 search for $pp \to Z + E_T$ with $Z \to \ell\ell$ at 13 TeV with 36.1 fb⁻¹ of data. Limits set for simplified models.

38 AABOUD 18A search for $pp \to t\bar{t} E_T$ or $pp \to b\bar{b} E_T$ at 13 TeV, 36.1 fb⁻¹ of data. Limits set for simplified models.

39 AABOUD 18CA search for $pp \to V\chi\chi$ with $V \to jj$ at 13 TeV, 36.1 fb⁻¹; no signal; limits set in m(DM) vs m(mediator) simplified model plane.

40 AABOUD 18I search for $pp \to j + E_T$ at 13 TeV with 36.1 fb⁻¹ of data. Limits set for simplified models with pair-produced weakly interacting dark-matter candidates.

41 AGUILAR-AREVALO 18b search for WIMP production in MiniBooNE p beam dump; no signal; limits set for m(χ) ~ 5–50 MeV in vector portal DM model.

42 KHACHATRYAN 18 search for $pp \to Z(\ell\ell) + E_T$; no signal; limits set on effective dark matter interactions and other exotic physics models.

43 SIRUNYAN 18B search for $pp \to t E_T$ at 13 TeV and 36 fb⁻¹; no signal; limits placed on DM models involving a flavor changing neutral current, scalar resonance decaying to top quark and DM.

44 SIRUNYAN 18B0 search for high mass dijet resonances at 13 TeV and 36 fb⁻¹; no signal: limits placed on various models, including simplified DM models involving a spin = 1 $z'$ mediator.

45 SIRUNYAN 18BV search for $pp \to Z E_T$ at 13 TeV; no signal, limits placed for various exotic physics models including DM.

46 SIRUNYAN 18C search for new physics in $pp \to$ final states with two oppositely charged leptons at 13 TeV with 35.9 fb⁻¹. Limits placed on m(mediator) and top squark for various simplified models.

47 SIRUNYAN 18CU search for $pp \to Z \bar{E}_T$ at 13 TeV and 2.3 fb⁻¹; no signal: limits placed for various exotic models including DM.

48 SIRUNYAN 18DH search for $pp \to \chi\chi h; h \to \gamma\gamma$ or $\tau\bar{\tau}$ at 13 TeV, 35.9 fb⁻¹; no signal; limits placed on massive boson mediator $Z'$ in the context of $Z' + 2HDM$ and baryonic $Z'$ models. Limits also cast in terms of spin-independent WIMP-nucleon cross section for masses 1–200 GeV.

49 SIRUNYAN 18S search for $pp \to jets E_T$ at 13 TeV; no signal: limits placed on simplified dark matter models, on the branching ratio of the Higgs boson to invisible particles, and on several other exotic physics models including fermion portal DM.

50 AABOUD 17A search for $H \to b\bar{b} + E_T$. See Fig. 4b for limits set on VB mediator vs WIMP mass.

51 AABOUD 17AM search for $pp \to Z' \to Ah \to h(b\bar{b}) + E_T$ at 13 TeV. Limits set in m(Z') vs. m(A) plane and on the visible cross section of $h(b\bar{b}) + E_T$ events in bins of $E_T$.

52 AABOUD 17AQ search for WIMP in $pp \to h(\gamma\gamma) + E_T$ in 36.1 fb⁻¹ of data. Limits on the visible cross section are also provided. Model dependent limits on spin independent DM - Nucleon cross-section are also presented, which are more stringent than those from direct searches for DM mass smaller than 2.5 GeV.

53 AABOUD 17BD search for $pp \to jet(s) + E_T$ at 13 TeV with 3.2 fb⁻¹ of data. Limits set for simplified models. Observables corrected for detector effects can be used to constrain other models.

54 AABOUD 17R, for an axial vector mediator in the s-channel, excludes $m(\text{mediator}) < 750–1200$ GeV for $m(\text{DM}) < 230–480$ GeV, depending on the couplings.

55 AGUILAR-AREVALO 17A search for DM produced in 8 GeV proton collisions with steel beam dump followed by DM-nucleon scattering in MiniBooNE detector. Limit placed on
<table><thead><tr><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td>ZHAO</td><td>13</td><td>PR D88 052004</td><td>W. Zhao et al. (CDEX Collab.)</td></tr><tr><td>AALTONEN</td><td>12K</td><td>PRL 108 201802</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>12M</td><td>PRL 108 211804</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>ABBASI</td><td>12</td><td>PR D85 042002</td><td>R. Abbasi et al. (IceCube Collab.)</td></tr><tr><td>ABRAMOWSKI</td><td>12</td><td>APJ 750 123</td><td>A. Abramowski et al. (H.E.S.S. Collab.)</td></tr><tr><td>ACKERMANN</td><td>12</td><td>PR D66 022002</td><td>M. Ackermann et al. (Fermi-LAT Collab.)</td></tr><tr><td>AKIMOV</td><td>12</td><td>PR B309 14</td><td>(ZEPLIN-II Collab.)</td></tr><tr><td>ALIU</td><td>12</td><td>PR D85 062001</td><td>E. Aliu et al. (VERITAS Collab.)</td></tr><tr><td>ANGLOHER</td><td>12</td><td>EPJ C72 1971</td><td>G. Angloher et al. (CRESST-II Collab.)</td></tr><tr><td>APRILE</td><td>12</td><td>PRL 109 181301</td><td>E. Aprile et al. (XENON100 Collab.)</td></tr><tr><td>ARCHAMBAU</td><td>12</td><td>PL B711 153</td><td>S. Archambault et al. (PICASSO Collab.)</td></tr><tr><td>ARMENGAUD</td><td>12</td><td>PR D66 051701</td><td>E. Armengaud et al. (EDELWEISS Collab.)</td></tr><tr><td>BARRETO</td><td>12</td><td>PL B711 264</td><td>J. Barreto et al. (DAMIC Collab.)</td></tr><tr><td>BEHNKE</td><td>12</td><td>PR D86 052001</td><td>E. Behnke et al. (COUPP Collab.)</td></tr><tr><td>Also</td><td>12</td><td>PR D90 079902 (errat.)</td><td>E. Behnke et al. (COUPP Collab.)</td></tr><tr><td>BROWN</td><td>12</td><td>PR D85 021301</td><td>A. Brown et al. (OXF)</td></tr><tr><td>CHATRCHYAN</td><td>12AP</td><td>PR JEP 1209 094</td><td>S. Chatrchyan et al. (CMS Collab.)</td></tr><tr><td>CHATRCHYAN</td><td>12T</td><td>PRL 108 261803</td><td>S. Chatrchyan et al. (CMS Collab.)</td></tr><tr><td>DAHL</td><td>12</td><td>PRL 108 259001</td><td>C.E. Dahl, J. Hall, W.H. Lippincott</td></tr><tr><td>DAW</td><td>12</td><td>ASP 35 397</td><td>E. Daw et al. (DRIFT-IID Collab.)</td></tr><tr><td>FELIZARDO</td><td>12</td><td>PRL 108 201302</td><td>M. Felizardo et al. (SIMPLE Collab.)</td></tr><tr><td>KIM</td><td>12</td><td>PRL 108 181301</td><td>S.C. Kim et al. (KIMS Collab.)</td></tr><tr><td>AALSETH</td><td>11</td><td>PR D85 131301</td><td>C. Aalseth et al. (CoGENT Collab.)</td></tr><tr><td>AALSETH</td><td>11A</td><td>PR 107 141301</td><td>C.E. Aalseth et al. (CoGENT Collab.)</td></tr><tr><td>ABBASI</td><td>11C</td><td>PR D84 022004</td><td>R. Abbasi et al. (IceCube Collab.)</td></tr><tr><td>ABRAMOWSKI</td><td>11</td><td>PRL 106 161301</td><td>A. Abramowski et al. (H.E.S.S. Collab.)</td></tr><tr><td>ACKERMANN</td><td>11</td><td>PRL 107 241302</td><td>M. Ackermann et al. (Fermi-LAT Collab.)</td></tr><tr><td>AHLEN</td><td>11</td><td>PR D86 051619</td><td>S. Ahlen et al. (DMTPC Collab.)</td></tr><tr><td>AHMED</td><td>11</td><td>PR D83 112002</td><td>Z. Ahmed et al. (CDMS Collab.)</td></tr><tr><td>AHMED</td><td>11A</td><td>PR D84 011102</td><td>Z. Ahmed et al. (CDMS and EDELWEISS Collabs.)</td></tr><tr><td>AHMED</td><td>11B</td><td>PRL 106 131302</td><td>Z. Ahmed et al. (CDMS Collab.)</td></tr><tr><td>AJELLO</td><td>11</td><td>PR D84 032007</td><td>M. Ajello et al. (Fermi-LAT Collab.)</td></tr><tr><td>ANGLE</td><td>11</td><td>PR D87 051301</td><td>J. Angle et al. (XENON10 Collab.)</td></tr><tr><td>Also</td><td>11</td><td>PRL 110 249901 (errat.)</td><td>Z. Ahmed et al. (XENON10 Collab.)</td></tr><tr><td>APRILE</td><td>11</td><td>PR D84 052003</td><td>E. Aprile et al. (XENON100 Collab.)</td></tr><tr><td>APRILE</td><td>11A</td><td>PR D84 061101</td><td>E. Aprile et al. (XENON100 Collab.)</td></tr><tr><td>APRILE</td><td>11B</td><td>PRL 107 131302</td><td>E. Aprile et al. (XENON100 Collab.)</td></tr><tr><td>ARMENGAUD</td><td>11</td><td>PL B702 329</td><td>E. Armengaud et al. (EDELWEISS-II Collab.)</td></tr><tr><td>ARMENGAUD</td><td>11</td><td>PL B706 185</td><td>E. Armengaud et al. (EDELWEISS-II Collab.)</td></tr><tr><td>BERGER-SA</td><td>11</td><td>PRL 107 241303</td><td>A. Geringer-Sameth, S.M. Koushiappas (COUPP Collab.)</td></tr><tr><td>HORN</td><td>11</td><td>PL B705 471</td><td>M. Horn et al. (ZEPLIN-II Collab.)</td></tr><tr><td>TANAKA</td><td>11</td><td>APJ 742 78</td><td>T. Tanaka et al. (Super-Kamiokande Collab.)</td></tr><tr><td>ABBASI</td><td>10</td><td>PR D81 057101</td><td>R. Abbasi et al. (IceCube Collab.)</td></tr><tr><td>AHMED</td><td>10</td><td>PR D86 051619</td><td>(CDMS II Collab.)</td></tr><tr><td>AKERIB</td><td>10</td><td>PR D82 122004</td><td>D.S. Akerib et al. (CDMS II Collab.)</td></tr><tr><td>AKIMOV</td><td>10</td><td>PL B692 180</td><td>Z.Yu. Akimov et al. (ZEPLIN-II Collab.)</td></tr><tr><td>APRILE</td><td>10</td><td>PRL 105 131302</td><td>E. Aprile et al. (XENON100 Collab.)</td></tr><tr><td>ARMENGAUD</td><td>10</td><td>PL B687 294</td><td>E. Armengaud et al. (EDELWEISS-II Collab.)</td></tr><tr><td>FELIZARDO</td><td>10</td><td>PL B611 211301</td><td>M. Felizardo et al. (The SIMPLE Collab.)</td></tr><tr><td>MIUCHI</td><td>10</td><td>PL B686 11</td><td>K. Miuchi et al. (NEWAGE Collab.)</td></tr><tr><td>ABBASI</td><td>09B</td><td>PRL 102 201302</td><td>R. Abbasi et al. (IceCube Collab.)</td></tr><tr><td>AHMED</td><td>09B</td><td>PRL 102 011301</td><td>Z. Ahmed et al. (CDMS Collab.)</td></tr><tr><td>ANGLE</td><td>09B</td><td>PR D80 115005</td><td>J. Angle et al. (XENON10 Collab.)</td></tr><tr><td>ANGLOHER</td><td>09B</td><td>ASP 31 270</td><td>G. Angloher et al. (CRESST Collab.)</td></tr><tr><td>ARCHAMBAU</td><td>09</td><td>PL B682 185</td><td>S. Archambault et al. (PICASSO Collab.)</td></tr><tr><td>LEBEDENKO</td><td>09A</td><td>PRL 103 151302</td><td>V.N. Lebedenko et al. (ZEPLIN-II Collab.)</td></tr><tr><td>LIN</td><td>09</td><td>PR D79 061101</td><td>S.T. Lin et al. (TEXON Collab.)</td></tr><tr><td>AALSETH</td><td>08</td><td>PRL 101 251301</td><td>C.E. Aalseth et al. (CoGENT Collab.)</td></tr><tr><td>Also</td><td>08A</td><td>PRL 101 091301</td><td>C.E. Aalseth et al. (CoGENT Collab.)</td></tr><tr><td>ANGLE</td><td>08</td><td>PR 101 091301</td><td>J. Angle et al. (XENON10 Collab.)</td></tr><tr><td>BEDNYAKOV</td><td>08</td><td>PAN 71 111</td><td>V.A. Bednyakov, H.P. Klapdor-Kleingrothaus, I.V. Krivosheina Translated from YAF 71 112.</td></tr><tr><td>ALNER</td><td>07</td><td>PL B653 161</td><td>G.J. Alner et al. (ZEPLIN-II Collab.)</td></tr><tr><td>LEE</td><td>07A</td><td>PRL 99 091301</td><td>H.S. Lee et al. (KIMS Collab.)</td></tr><tr><td>MIUCHI</td><td>07</td><td>PL B654 58</td><td>K. Miuchi et al. (CDMS Collab.)</td></tr><tr><td>AKERIB</td><td>06</td><td>PR D73 011102</td><td>D.S. Akerib et al. (CDMS Collab.)</td></tr><tr><td>SHIMIZU</td><td>06A</td><td>PL B633 195</td><td>Y. Shimizu et al. (CDMS Collab.)</td></tr><tr><td>AKERIB</td><td>05</td><td>PR D72 052009</td><td>D.S. Akerib et al. (UK Dark Matter Collab.)</td></tr><tr><td>ALNER</td><td>05</td><td>PL B616 17</td><td>G.J. Alner et al. (PICASSO Collab.)</td></tr><tr><td>BARNABE-HE</td><td>05</td><td>PR D624 186</td><td>M. Barnabe-Heider et al. (EDELWEISS Collab.)</td></tr><tr><td>BENOIT</td><td>05</td><td>PL B616 25</td><td>A. Benoit et al. (SIMPLE Collab.)</td></tr><tr><td>GIRARD</td><td>05</td><td>PL B621 233</td><td>T.A. Girard et al. (SIMPLE Collab.)</td></tr><tr><td>GIULIANI</td><td>05</td><td>PRL 95 101301</td><td>F. Giuliani</td></tr><tr><td>GIULIANI</td><td>05A</td><td>PR D71 123503</td><td>F. Giuliani, T.A. Girard</td></tr><tr><td>KLAPDOR-K</td><td>05</td><td>PL B609 226</td><td>H.V. Klapdor-Kleingrothaus, I.V. Krivosheina, C. Tomei</td></tr><tr><td>GIULIANI</td><td>04</td><td>PL B588 151</td><td>F. Giuliani</td></tr><tr><td>GIULIANI</td><td>04A</td><td>PRL 93 161301</td><td>F. Giuliani</td></tr><tr><td>MIUCHI</td><td>03</td><td>ASP 19 135</td><td>K. Miuchi et al. (CDMS Collab.)</td></tr><tr><td>TAKEDA</td><td>03</td><td>PL B572 145</td><td>A. Takeda et al. (CRESST Collab.)</td></tr><tr><td>ANGLOHER</td><td>02</td><td>ASP 18 43</td><td>P. Belli et al. (DAMA Collab.)</td></tr><tr><td>BELL</td><td>02</td><td>PR D66 043503</td><td>A. Benoit et al. (EDELWEISS Collab.)</td></tr><tr><td>BERNABEI</td><td>02C</td><td>EPJ C23 61</td><td>R. Bernabei et al. (DAMA Collab.)</td></tr><tr><td>GREEN</td><td>02</td><td>PR D66 083003</td><td>A.M. Green</td></tr><tr><td>BAUDIS</td><td>01</td><td>PR D63 022001</td><td>L. Baudis et al. (Heidelberg-Moscow Collab.)</td></tr><tr><td>SMITH</td><td>01</td><td>PR D64 0643502</td><td>D. Smith, N. Weiner</td></tr><tr><td>JHEP</td><td>01</td><td>PR D61 01044</td><td>P. U. M. M. Kamionkowski, P. Vogel</td></tr><tr><td>BENOIT</td><td>00</td><td>PL B479 8</td><td>A. Benoit et al. (EDELWEISS Collab.)</td></tr><tr><td>BERNABEI</td><td>00D</td><td>NJP 2 15</td><td>R. Bernabei et al. (DAMA Collab.)</td></tr><tr><td>COLLAR</td><td>00</td><td>PRL 85 3083</td><td>J.J. Collar et al. (SIMPLE Collab.)</td></tr><tr><td>AMBROSIO</td><td>99</td><td>PR D60 080200</td><td>M. Ambrosio et al. (Macro Collab.)</td></tr><tr><td>BERNABEI</td><td>99</td><td>PR B450 448</td><td>R. Bernabei et al. (DAMA Collab.)</td></tr><tr><td>BERNABEI</td><td>99D</td><td>PR B3 4918</td><td>R. Bernabei et al. (DAMA Collab.)</td></tr><tr><td>BRHLIK</td><td>99</td><td>PL B464 303</td><td>M. Brhlik, L. Roszkowski</td></tr><tr><td>DERBIN</td><td>99</td><td>PAN 62 1886</td><td>A.V. Derbin et al. (DAMA Collab.)</td></tr><tr><td>KLIMENKO</td><td>98</td><td>Transl. from YAF 62 2034.</td><td>A.A. Klimenko et al. Translated from ZETF 67 875.</td></tr><tr><td>SARSA</td><td>97</td><td>PR D56 1856</td><td>M.L. Sarsa et al. (ZARA)</td></tr><tr><td>ALESSAND</td><td>96</td><td>PL B384 316</td><td>A. Alessandrello et al. (MILA, MILAI, SASSO)</td></tr><tr><td>BELL</td><td>96</td><td>PL B387 222</td><td>P. Belli et al. (DAMA Collab.)</td></tr><tr><td>Also</td><td>96</td><td>PL B389 783 (errat.)</td><td>P. Belli et al. (DAMA Collab.)</td></tr><tr><td>BELL</td><td>96C</td><td>NC C19 537</td><td>P. Belli et al. (DAMA Collab.)</td></tr><tr><td>BERNABEI</td><td>96</td><td>PL B389 757</td><td>R. Bernabei et al. (DAMA Collab.)</td></tr><tr><td>COLLAR</td><td>96</td><td>PRL 76 331</td><td>J.J. Collar (SCUC)</td></tr><tr><td>SARSA</td><td>96</td><td>PL B386 458</td><td>M.L. Sarsa et al. (ZARA)</td></tr><tr><td>Also</td><td>96</td><td>PR D56 18556</td><td>M.L. Sarsa et al. (ZARA)</td></tr><tr><td>SMITH</td><td>96</td><td>PL B379 299</td><td>P.F. Fajardo et al. (RAL, SHEF, LOIC+)</td></tr><tr><td>SNOWDEN</td><td>96</td><td>PRL 76 332</td><td>D.P. Snowden-Ift, E.S. Freeman, P.B. Price (UCB)</td></tr><tr><td>GARCIA</td><td>95</td><td>PRL D51 1458</td><td>E. Garcia et al. (ZARA, SCUC, PNL)</td></tr><tr><td>QUENBY</td><td>95</td><td>PL B351 70</td><td>J.J. Quenby et al. (LOIC, RAL, SHEF+)</td></tr><tr><td>SNOWDEN</td><td>95</td><td>PRL 74 4133</td><td>D.P. Snowden-Ift, E.S. Freeman, P.B. Price (UCB)</td></tr><tr><td>Also</td><td>95</td><td>PRL 76 331</td><td>J.J. Collar (SCUC)</td></tr><tr><td>Also</td><td>95</td><td>PRL 76 332</td><td>D.P. Snowden-Ift, E.S. Freeman, P.B. Price (UCB)</td></tr><tr><td>BECK</td><td>94</td><td>PRL B336 141</td><td>M. Beck et al. (MPIK, KIAE, SASSO)</td></tr><tr><td>BACCI</td><td>92</td><td>PL B293 460</td><td>C. Bacci et al. (Beijing-Roma-Saclay Collab.)</td></tr><tr><td>REUSSER</td><td>91</td><td>PL B255 143</td><td>D. Reusser et al. (NEUC, CIT, PSI)</td></tr><tr><td>CALDWELL</td><td>88</td><td>PRL 61 510</td><td>D.O. Caldwell et al. (UCSB, UCB, LBL)</td></tr></tbody></table>

## Other Particle Searches

OMITTED FROM SUMMARY TABLE
OTHER PARTICLE SEARCHES

Revised February 2018 by K. Hikasa (Tohoku University).

We collect here those searches which do not appear in any other search categories. These are listed in the following order:

* Concentration of stable particles in matter

* General new physics searches

* Limits on jet-jet resonance in hadron collisions

* Limits on neutral particle production at accelerators

* Limits on charged particles in $e^+e^-$ collisions

* Limits on charged particles in hadron reactions

* Limits on charged particles in cosmic rays

* Searches for quantum black hole production

Note that searches appear in separate sections elsewhere for Higgs bosons (and technipions), other heavy bosons (including $W_R$, $W'$, $Z'$, leptoquarks, axigluons), axions (including pseudo-Goldstone bosons, Majorons, familons), WIMPs, heavy leptons, heavy neutrinos, free quarks, monopoles, supersymmetric particles, and compositeness.

We no longer list for limits on tachyons and centauros. See our 1994 edition for these limits.

## CONCENTRATION OF STABLE PARTICLES IN MATTER

### Concentration of Heavy (Charge +1) Stable Particles in Matter

<table><thead><tr><th>VALUE</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;4 × 10<sup>-17</sup></td><td>95</td><td>1 YAMAGATA</td><td>93</td><td>Deep sea water, M=5-1600m<sub>p</sub></td></tr><tr><td>&lt;6 × 10<sup>-15</sup></td><td>95</td><td>2 VERKERK</td><td>92</td><td>SPEC Water, M=10<sup>5</sup> to 3 × 10<sup>7</sup> GeV</td></tr><tr><td>&lt;7 × 10<sup>-15</sup></td><td>95</td><td>2 VERKERK</td><td>92</td><td>SPEC Water, M=10<sup>4</sup>, 6 × 10<sup>7</sup> GeV</td></tr><tr><td>&lt;9 × 10<sup>-15</sup></td><td>95</td><td>2 VERKERK</td><td>92</td><td>SPEC Water, M=10<sup>8</sup> GeV</td></tr><tr><td>&lt;3 × 10<sup>-23</sup></td><td>90</td><td>3 HEMMICK</td><td>90</td><td>SPEC Water, M = 1000m<sub>p</sub></td></tr><tr><td>&lt;2 × 10<sup>-21</sup></td><td>90</td><td>3 HEMMICK</td><td>90</td><td>SPEC Water, M = 5000m<sub>p</sub></td></tr><tr><td>&lt;3 × 10<sup>-20</sup></td><td>90</td><td>3 HEMMICK</td><td>90</td><td>SPEC Water, M = 10000m<sub>p</sub></td></tr><tr><td>&lt;1 × 10<sup>-29</sup></td><td>SMITH</td><td>82B</td><td>SPEC Water, M=30-400m<sub>p</sub></td></tr><tr><td>&lt;2 × 10<sup>-28</sup></td><td>SMITH</td><td>82B</td><td>SPEC Water, M=12-1000m<sub>p</sub></td></tr><tr><td>&lt;1 × 10<sup>-14</sup></td><td>SMITH</td><td>82B</td><td>SPEC Water, M>1000m<sub>p</sub></td></tr><tr><td>&lt;(0.2-1.) × 10<sup>-21</sup></td><td>SMITH</td><td>79</td><td>SPEC Water, M=6-350 m<sub>p</sub></td></tr></tbody></table>

¹ YAMAGATA 93 used deep sea water at 4000 m since the concentration is enhanced in deep sea due to gravity.

² VERKERK 92 looked for heavy isotopes in sea water and put a bound on concentration of stable charged massive particle in sea water. The above bound can be translated into a bound on charged dark matter particle ($5 \times 10^6$ GeV), assuming the local density, $\rho=0.3$ GeV/cm³, and the mean velocity ($\nu=300$ km/s).

³ See HEMMICK 90 Fig. 7 for other masses 100-10000 $m_p$.

### Concentration of Heavy Stable Particles Bound to Nuclei

<table><thead><tr><th>VALUE</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 2 × 10<sup>-17</sup>/nucleon</td><td>95</td><td>1 AFEK</td><td>21</td><td>millicharged particle search</td></tr><tr><td>&lt;1.2 × 10<sup>-11</sup></td><td>95</td><td>2 JAVORSEK</td><td>01 SPEC Au, M= 3 GeV</td></tr><tr><td>&lt;6.9 × 10<sup>-10</sup></td><td>95</td><td>2 JAVORSEK</td><td>01 SPEC Au, M= 144 GeV</td></tr><tr><td>&lt;1 × 10<sup>-11</sup></td><td>95</td><td>3 JAVORSEK</td><td>01B SPEC Au, M= 188 GeV</td></tr><tr><td>&lt;1 × 10<sup>-8</sup></td><td>95</td><td>3 JAVORSEK</td><td>01B SPEC Au, M= 1669 GeV</td></tr><tr><td>&lt;6 × 10<sup>-9</sup></td><td>95</td><td>3 JAVORSEK</td><td>01B SPEC Fe, M= 188 GeV</td></tr><tr><td>&lt;1 × 10<sup>-8</sup></td><td>95</td><td>3 JAVORSEK</td><td>01B SPEC Fe, M= 647 GeV</td></tr><tr><td>&lt;4 × 10<sup>-20</sup></td><td>90</td><td>4 HEMMICK</td><td>90 SPEC C, M = 100m<sub>p</sub></td></tr><tr><td>&lt;8 × 10<sup>-20</sup></td><td>90</td><td>4 HEMMICK</td><td>90 SPEC C, M = 1000m<sub>p</sub></td></tr><tr><td>&lt;2 × 10<sup>-16</sup></td><td>90</td><td>4 HEMMICK</td><td>90 SPEC C, M = 10000m<sub>p</sub></td></tr><tr><td>&lt;6 × 10<sup>-13</sup></td><td>90</td><td>4 HEMMICK</td><td>90 SPEC Li, M = 1000m<sub>p</sub></td></tr><tr><td>&lt;1 × 10<sup>-11</sup></td><td>90</td><td>4 HEMMICK</td><td>90 SPEC Be, M = 1000m<sub>p</sub></td></tr><tr><td>&lt;6 × 10<sup>-14</sup></td><td>90</td><td>4 HEMMICK</td><td>90 SPEC B, M = 1000m<sub>p</sub></td></tr></tbody></table>
<table><tr><td>&lt;4 &times; 10<sup>-17</sup></td><td>90</td><td><sup>4</sup>HEMMICK</td><td>90</td><td>SPEC</td><td>O, M = 1000m<sub>p</sub></td></tr><tr><td>&lt;4 &times; 10<sup>-15</sup></td><td>90</td><td><sup>4</sup>HEMMICK</td><td>90</td><td>SPEC</td><td>F, M = 1000m<sub>p</sub></td></tr><tr><td>&lt; 1.5 &times; 10<sup>-13</sup>/nucleon</td><td>68</td><td><sup>5</sup> NORMAN</td><td>89</td><td>SPEC</td><td>206<sup>...</sup>PbX<sup>-</sup></td></tr><tr><td>&lt; 1.2 &times; 10<sup>-12</sup>/nucleon</td><td>68</td><td><sup>5</sup> NORMAN</td><td>87</td><td>SPEC</td><td>56,58<sup>...</sup>FeX<sup>-</sup></td></tr></table>

¹ AFEK 21 search for millicharged particles bound to matter using an optomechanical device. No signal was observed. Limits placed in the abundance vs. charge plane (Fig. 3). This is translated to the mass versus charge plane by requiring bound states to be stable.

² JAVORSEK 01 search for (neutral) SIMPs (strongly interacting massive particles) bound to Au nuclei. Here M is the effective SIMP mass.

³ JAVORSEK 01B search for (neutral) SIMPs (strongly interacting massive particles) bound to Au and Fe nuclei from various origins with exposures on the earth's surface, in a satellite, heavy ion collisions, etc. Here M is the mass of the anomalous nucleus. See also JAVORSEK 02.

⁴ See HEMMICK 90 Fig. 7 for other masses 100–10000 $m_p$.

⁵ Bound valid up to $m_X$ ~ 100 TeV.

## GENERAL NEW PHYSICS SEARCHES

This subsection lists some of the search experiments which look for general signatures characteristic of new physics, independent of the framework of a specific model.

The observed events are compatible with Standard Model expectation, unless noted otherwise.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td>We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td></td><td>1 ALKHATIB</td><td>21A</td><td>SCDM CDMSlite search for fractionally charged relics</td></tr><tr><td></td><td>2 AGUILAR-AR...20B</td><td>20B</td><td>CONN ν elastic scatter on nuclei</td></tr><tr><td></td><td>3 FEDDERKE</td><td>20</td><td>CHAMPS from white dwarfs</td></tr><tr><td></td><td>4 SIRUNYAN</td><td>20A</td><td>CMS SUSY/LQ search with mT2 or long-lived charged particles</td></tr><tr><td></td><td>5 ALCANTARA</td><td>19</td><td>Auger, superheavy DM</td></tr><tr><td></td><td>6 PORAYKO</td><td>18</td><td>PPTA pulsar timing fuzzy DM search</td></tr><tr><td></td><td>7 AAD</td><td>15AT</td><td>ATLS t + E<sub>T</sub></td></tr><tr><td></td><td>8 KHACHATRY...15F</td><td>CMS</td><td>t + E<sub>T</sub></td></tr><tr><td></td><td>9 AALTONEN</td><td>14J</td><td>CDF W + 2 jets</td></tr><tr><td></td><td>10 AAD</td><td>13A</td><td>ATLS W W → ℓνℓ'ν</td></tr><tr><td></td><td>11 AAD</td><td>13C</td><td>ATLS γ + E<sub>T</sub></td></tr><tr><td></td><td>12 AALTONEN</td><td>13I</td><td>CDF Delayed γ + E<sub>T</sub></td></tr><tr><td></td><td>13 CHATRCHYAN13</td><td>CMS</td><td>ℓ<sup>+</sup>ℓ<sup>-</sup> + jets + E<sub>T</sub></td></tr><tr><td></td><td>14 AAD</td><td>12C</td><td>ATLS t<span style="text-decoration: overline">t</span> + E<sub>T</sub></td></tr><tr><td></td><td>15 AALTONEN</td><td>12M</td><td>CDF jet + E<sub>T</sub></td></tr><tr><td></td><td>16 CHATRCHYAN12AP</td><td>CMS</td><td>jet + E<sub>T</sub></td></tr><tr><td></td><td>17 CHATRCHYAN12Q</td><td>CMS</td><td>Z + jets + E<sub>T</sub></td></tr><tr><td></td><td>18 CHATRCHYAN12T</td><td>CMS</td><td>γ + E<sub>T</sub></td></tr><tr><td></td><td>19 AAD</td><td>11S</td><td>ATLS jet + E<sub>T</sub></td></tr><tr><td></td><td>20 AALTONEN</td><td>11AF</td><td>CDF ℓ<sup>±</sup>ℓ<sup>±</sup></td></tr><tr><td></td><td>21 CHATRCHYAN11C</td><td>CMS</td><td>ℓ<sup>+</sup>ℓ<sup>-</sup> + jets + E<sub>T</sub></td></tr><tr><td></td><td>22 CHATRCHYAN11U</td><td>CMS</td><td>jet + E<sub>T</sub></td></tr><tr><td></td><td>23 AALTONEN</td><td>10AF</td><td>CDF γγ + ℓ, E<sub>T</sub></td></tr><tr><td></td><td>24 AALTONEN</td><td>09AF</td><td>CDF ℓγb E<sub>T</sub></td></tr><tr><td></td><td>25 AALTONEN</td><td>09G</td><td>CDF ℓℓℓ E<sub>T</sub></td></tr></tbody></table>

¹ ALKHATIB 21A search for lightly ionizing fractionally charged relics scattering from Ge. No signal observed. Limits plotted in fractional charge f vs. vertical intensity plane for m ~ 5 MeV to 100 TeV.

² AGUILAR-AREVALO 20B search for light BSM mediator effect on ν elastic scatter on nuclei; no signal; limits placed in m(mediator) vs. coupling plane for two models of MeV-scale mediators.

³ FEDDERKE 20 place limits on cosmic relic charged massive particles (CHAMPS) due to their capture and subsequent disruption of old white dwarf stars; limits placed in the m(CHAMP) vs. relic density parameter plane.

⁴ SIRUNYAN 20A search for SUSY and LQ production using mT2 or presence of long-lived charged particle; no signal, limits placed in various mass planes for different BSM scenarios and various assumed lifetimes.

⁵ ALCANTARA 19 place limits on m(WIMPzilla=X) vs lifetime from upper bound on ultra high energy cosmic rays at Auger experiment: e.g. $\tau(X) < 4 \times 10^{22}$ yr for m(X) = $10^{16}$ GeV.

⁶ PORAYKO 18 search for deviations in the residuals of pulsar timing data using PPTA. No signal observed. Limits set on fuzzy DM with $3 \times 10^{-24} < m(DM) < 2 \times 10^{-22}$ eV.

⁷ AAD 15AT search for events with a top quark and missing $E_T$ in pp collisions at $E_{cm} = 8$ TeV with $L = 20.3$ fb⁻¹.

⁸ KHACHATRYAN 15F search for events with a top quark and missing $E_T$ in pp collisions at $E_{cm} = 8$ TeV with $L = 19.7$ fb⁻¹.

⁹ AALTONEN 14J examine events with a W and two jets in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 8.9$ fb⁻¹. Invariant mass distributions of the two jets are consistent with the Standard Model expectation.

¹⁰ AAD 13A search for resonant W W production in pp collisions at $E_{cm} = 7$ TeV with $L = 4.7$ fb⁻¹.

¹¹ AAD 13C search for events with a photon and missing $E_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 4.6$ fb⁻¹.

¹² AALTONEN 13i search for events with a photon and missing $E_T$, where the photon is detected after the expected timing, in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 6.3$ fb⁻¹. The data are consistent with the Standard Model expectation.

¹³ CHATRCHYAN 13 search for events with an opposite-sign lepton pair, jets, and missing $E_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 4.98$ fb⁻¹.

¹⁴ AAD 12C search for events with a $t\bar{t}$ pair and missing $\ell_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 1.04$ fb⁻¹.

¹⁵ AALTONEN 12M search for events with a jet and missing $E_T$ in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 6.7$ fb⁻¹.

¹⁶ CHATRCHYAN 12AP search for events with a jet and missing $E_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 5.0$ fb⁻¹.

¹⁷ CHATRCHYAN 12Q search for events with a Z, jets, and missing $\ell_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 4.98$ fb⁻¹.

¹⁸ CHATRCHYAN 12T search for events with a photon and missing $\ell_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 5.0$ fb⁻¹.

¹⁹ AAD 11S search for events with one jet and missing $E_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 33$ fb⁻¹.

²⁰ AALTONEN 11AF search for high-$p_T$ like-sign dileptons in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 6.1$ fb⁻¹.

²¹ CHATRCHYAN 11C search for events with an opposite-sign lepton pair, jets, and missing $E_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 34$ fb⁻¹.

²² CHATRCHYAN 11U search for events with one jet and missing $E_T$ in pp collisions at $E_{cm} = 7$ TeV with $L = 36$ fb⁻¹.

²³ AALTONEN 10AF search for $\gamma\gamma$ events with $e, \mu, \tau$, or missing $E_T$ in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 1.1-2.0$ fb⁻¹.

²⁴ AALTONEN 09AF search for $\ell\gamma b$ events with missing $E_T$ in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 1.9$ fb⁻¹. The observed events are compatible with Standard Model expectation including $t\bar{t}\gamma$ production.

²⁵ AALTONEN 09G search for $\mu\mu\mu$ and $\mu\mu e$ events with missing $E_T$ in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 976$ pb⁻¹.

## LIMITS ON JET-JET RESONANCES

### Heavy Particle Production Cross Section

Limits are for a particle decaying to two hadronic jets.

<table><thead><tr><th>Units/pb)</th><th>CL%</th><th>Mass/GeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td></td><td></td><td>We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td></td><td></td><td></td><td>1 TUMASYAN</td><td>23L</td><td>CMS dijet resonance in 4-jet events</td></tr><tr><td></td><td></td><td></td><td>2 AAD</td><td>20AD</td><td>ATLS pp at 13 TeV, dijet resonance</td></tr><tr><td></td><td></td><td></td><td>3 AAD</td><td>20T</td><td>ATLS dijet resonance search</td></tr><tr><td></td><td></td><td></td><td>4 AAD</td><td>20W</td><td>ATLS dijet resonance plus lepton</td></tr><tr><td></td><td></td><td></td><td>5 SIRUNYAN</td><td>20AI</td><td>CMS dijet resonance search</td></tr><tr><td></td><td></td><td></td><td>6 AABOUD</td><td>19AJ</td><td>ATLS pp → γX, X → jj</td></tr><tr><td></td><td></td><td></td><td>7 SIRUNYAN</td><td>19B</td><td>CMS pp → jA, A → bD</td></tr><tr><td></td><td></td><td></td><td>8 SIRUNYAN</td><td>19CD</td><td>CMS pp → Z'γ, Z' → jj</td></tr><tr><td></td><td></td><td></td><td>9 AABOUD</td><td>18AD</td><td>ATLS pp → Y → HX → (bb) + (qq)</td></tr><tr><td></td><td></td><td></td><td>10 AABOUD</td><td>18CK</td><td>ATLS pp → bbb + E<sub>T</sub></td></tr><tr><td></td><td></td><td></td><td>11 AABOUD</td><td>18CL</td><td>ATLS pp → vector-like quarks</td></tr><tr><td></td><td></td><td></td><td>12 AABOUD</td><td>18N</td><td>ATLS pp → jj resonance</td></tr><tr><td></td><td></td><td></td><td>13 SIRUNYAN</td><td>18DJ</td><td>CMS pp → ZZ or WZ → ℓ<span style="text-decoration: overline">t</span>jj</td></tr><tr><td></td><td></td><td></td><td>14 SIRUNYAN</td><td>18DY</td><td>CMS pp → RR; R → jj</td></tr><tr><td></td><td></td><td></td><td>15 KHACHATRY...17W</td><td>CMS</td><td>pp → jj resonance</td></tr><tr><td></td><td></td><td></td><td>16 KHACHATRY...17Y</td><td>CMS</td><td>pp → (8-10) j + E<sub>T</sub></td></tr><tr><td></td><td></td><td></td><td>17 SIRUNYAN</td><td>17F</td><td>CMS pp → jj angular distribution</td></tr><tr><td></td><td></td><td></td><td>18 AABOUD</td><td>16</td><td>ATLS pp → b + jet</td></tr><tr><td></td><td></td><td></td><td>19 AAD</td><td>16N</td><td>ATLS pp → 3 high E<sub>T</sub> jets</td></tr><tr><td></td><td></td><td></td><td>20 AAD</td><td>16S</td><td>ATLS pp → jj resonance</td></tr><tr><td></td><td></td><td></td><td>21 KHACHATRY...16K</td><td>CMS</td><td>pp → jj resonance</td></tr><tr><td></td><td></td><td></td><td>22 KHACHATRY...16L</td><td>CMS</td><td>pp → jj resonance</td></tr><tr><td></td><td></td><td></td><td>23 AAD</td><td>13D</td><td>ATLS 7 TeV pp → 2 jets</td></tr><tr><td></td><td></td><td></td><td>24 AALTONEN</td><td>13R</td><td>CDF 1.96 TeV p<span style="text-decoration: overline">p</span> → 4 jets</td></tr><tr><td></td><td></td><td></td><td>25 CHATRCHYAN13A</td><td>CMS</td><td>7 TeV pp → 2 jets</td></tr><tr><td></td><td></td><td></td><td>26 CHATRCHYAN13A</td><td>CMS</td><td>7 TeV pp → b<span style="text-decoration: overline">b</span>X</td></tr><tr><td></td><td></td><td></td><td>27 AAD</td><td>12S</td><td>ATLS 7 TeV pp → 2 jets</td></tr><tr><td></td><td></td><td></td><td>28 CHATRCHYAN12BL</td><td>CMS</td><td>7 TeV pp → t<span style="text-decoration: overline">t</span>X</td></tr><tr><td></td><td></td><td></td><td>29 AAD</td><td>11AG</td><td>ATLS 7 TeV pp → 2 jets</td></tr><tr><td></td><td></td><td></td><td>30 AALTONEN</td><td>11M</td><td>CDF 1.96 TeV p<span style="text-decoration: overline">p</span> → W + 2 jets</td></tr><tr><td></td><td></td><td></td><td>31 ABAZOV</td><td>11I</td><td>D0 1.96 TeV p<span style="text-decoration: overline">p</span> → W + 2 jets</td></tr><tr><td></td><td></td><td></td><td>32 AAD</td><td>10</td><td>ATLS 7 TeV pp → 2 jets</td></tr><tr><td></td><td></td><td></td><td>33 KHACHATRY...10</td><td>CMS</td><td>7 TeV pp → 2 jets</td></tr><tr><td></td><td></td><td></td><td>34 ABE</td><td>99F</td><td>CDF 1.8 TeV p<span style="text-decoration: overline">p</span> → b<span style="text-decoration: overline">b</span>+ anything</td></tr><tr><td></td><td></td><td></td><td>35 ABE</td><td>97G</td><td>CDF 1.8 TeV p<span style="text-decoration: overline">p</span> → 2 jets</td></tr><tr><td></td><td></td><td></td><td>36 ABE</td><td>93G</td><td>CDF 1.8 TeV p<span style="text-decoration: overline">p</span> → 2 jets</td></tr><tr><td></td><td></td><td></td><td>36 ABE</td><td>93G</td><td>CDF 1.8 TeV p<span style="text-decoration: overline">p</span> → 2 jets</td></tr><tr><td></td><td></td><td></td><td>36 ABE</td><td>93G</td><td>CDF 1.8 TeV p<span style="text-decoration: overline">p</span> → 2 jets</td></tr></tbody></table>

¹ TUMASYAN 23L search for dijet resonance in 4-jet events with 138 fb⁻¹ fb of data. There are two events in the tails of the distributions, each with a four-jet mass of 8 TeV and an average dijet mass of 2 TeV, resulting in local and global significances of 3.9 and 1.6 standard deviations, respectively, if interpreted as a signal. Limits set for simplified diquark model.

² AAD 20AD search for weakly supervised dijet resonance in ATLAS with 139 fb⁻¹ at 13 TeV; no signal; various limits placed depending on kinematics and production cross section.

³ AAD 20T search for dijet resonance with or without b-jets at 13 TeV and 139 fb⁻¹; no signal; limits placed in $\sigma$-BF vs mass plane for various BSM models.

⁴ AAD 20W search for dijet resonance plus lepton with ATLAS at 13 TeV and 139 fb⁻¹; no signal; limits placed in $\sigma$-BF vs mass plane for various BSM models.

⁵ SIRUNYAN 20AI search for dijet resonance in CMS at 13 TeV with 137 fb⁻¹; no signal; limits set in $\sigma$ vs. mass plane for various BSM models.
# Searches Particle Listings

## Other Particle Searches

⁶ AABOUD 19A search for low mass dijet resonance in $pp \to \gamma X, X \to jj$ at 13 TeV with 79.8 fb⁻¹ of data; no signal found; limits placed on $Z'$ model in coupling vs. $m(Z')$ plane.

⁷ SIRUNYAN 19B search for low mass resonance $pp \to jA, A \to b\bar{b}$ at 13 TeV using 35.9 fb⁻¹; no signal; exclude resonances 50–350 GeV depending on production and decay.

⁸ SIRUNYAN 19CD search for $pp \to Z'\gamma, Z' \to jj$ with fat jet (jj); no signal, limits placed in $m(Z')$ vs. coupling plane for $Z'$ masses from 10 to 125 GeV.

⁹ AABOUD 18AD search for new heavy particle $Y \to HX \to (bb) + (qq)$. No signal observed. Limits set on $m(Y)$ vs. $m(X)$ in the ranges of $m(Y)$ in 1–4 TeV and $m(X)$ in 50–1000 GeV.

¹⁰ AABOUD 18CK search for SUSY Higgsinos in gauge-mediation via $pp \to bbb + \bar{E}_T$ at 13 TeV using two complementary analyses with 24.3/36.1 fb⁻¹; no signal is found and Higgsinos with masses between 130 and 230 GeV and between 290 and 880 GeV are excluded at the 95% confidence level.

¹¹ AABOUD 18CL search for $pp \to$ vector-like quarks $\to$ jets at 13 TeV with 36 fb⁻¹; no signal seen; limits set on various VLQ scenarios. For pure $B \to Hb$ or $T \to Ht$, set the mass limit $m > 1010$ GeV.

¹² AABOUD 18n search for dijet resonance at Atlas with 13 TeV and 29.3 fb⁻¹; limits set on $m(Z')$ in the mass range of 450–1800 GeV.

¹³ SIRUNYAN 18DJ search for $pp \to ZZ$ or $WZ \to \ell\bar{\ell}jj$ resonance at 13 TeV, 35.9 fb⁻¹; no signal; limits set in the 400–4500 GeV mass range, exclusion of $W'$ up to 2270 GeV in the HVT model A, and up to 2330 GeV for HVT model B. WED bulk graviton exclusion up to 925 GeV.

¹⁴ SIRUNYAN 18DY search for $pp \to RR; R \to jj$ two dijet resonances at 13 TeV 35.9 fb⁻¹; no signal; limits placed on RPV top-quark pair production.

¹⁵ KHACHATRYAN 17W search for dijet resonance in 12.9 fb⁻¹ data at 13 TeV; see Fig. 2 for limits on axigluons, diquarks, dark matter mediators etc.

¹⁶ KHACHATRYAN 17Y search for $pp \to (8-10)j$ in 19.7 fb⁻¹ at 8 TeV. No signal seen. Limits set on colorons, axigluons, RPV, and SUSY.

¹⁷ SIRUNYAN 17F measure $pp \to jj$ angular distribution in 2.6 fb⁻¹ at 13 TeV; limits set on LEDs and quantum black holes.

¹⁸ AABOUD 16 search for resonant dijets including one or two $b$-jets with 3.2 fb⁻¹ at 13 TeV; exclude excited $b^*$ quark from 1.1–2.1 TeV; exclude leptophilic $Z'$ with SM couplings from 1.1–1.5 TeV.

¹⁹ AAD 16n search for $\ge 3$ jets with 3.6 fb⁻¹ at 13 TeV; limits placed on micro black holes (Fig. 10) and string balls (Fig. 11).

²⁰ AAD 16s search for high mass jet-jet resonance with 3.6 fb⁻¹ at 13 TeV; exclude portions of excited quarks, $W'$, $Z'$ and contact interaction parameter space.

²¹ KHACHATRYAN 16k search for dijet resonance in 2.4 fb⁻¹ data at 13 TeV; see Fig. 3 for limits on axigluons, diquarks etc.

²² KHACHATRYAN 16L use data scouting technique to search for $jj$ resonance on 18.8 fb⁻¹ of data at 8 TeV. Limits on the coupling of a leptophobic $Z'$ to quarks are set, improving on the results by other experiments in the mass range between 500–800 GeV.

²³ AAD 13D search for dijet resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 4.8$ fb⁻¹. The observed events are compatible with Standard Model expectation. See their Fig. 6 and Table 2 for limits on resonance cross section in the range $m = 1.0–4.0$ GeV.

²⁴ AALTONEN 13r search for production of a pair of jet-jet resonances in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 6.6$ fb⁻¹. See their Fig. 5 and Tables I, II for cross section limits.

²⁵ CHATRYCHAN 13A search for $qq, qg$, and $gg$ resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 4.8$ fb⁻¹. See their Fig. 3 and Table 1 for limits on resonance cross section in the range $m = 1.0–4.3$ TeV.

²⁶ CHATRYCHAN 13A search for $b\bar{b}$ resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 4.8$ fb⁻¹. See their Fig. 8 and Table 4 for limits on resonance cross section in the range $m = 1.0–4.0$ TeV.

²⁷ AAD 12s search for dijet resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 1.0$ fb⁻¹. See their Fig. 3 and Table 2 for limits on resonance cross section in the range $m = 0.9–4.0$ TeV.

²⁸ CHATRYCHAN 12BL search for $t\bar{t}$ resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 4.4$ fb⁻¹. See their Fig. 4 for limits on resonance cross section in the range $m = 0.5–3.0$ TeV.

²⁹ AAD 11AG search for dijet resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 36$ pb⁻¹. Limits on number of events for $m = 0.6–4$ TeV are given in their Table 3.

³⁰ AALTONEN 11m find a peak in two jet invariant mass distribution around 140 GeV in $W + 2$ jet events in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 4.3$ fb⁻¹.

³¹ ABAZOV 11I search for two-jet resonances in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 4.3$ fb⁻¹ and give limits $\sigma < (2.6–1.3)$ pb (95% CL) for $m = 110–170$ GeV. The result is incompatible with AALTONEN 11m.

³² AAD 10 search for narrow dijet resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 315$ nb⁻¹. Limits on the cross section in the range $10–10^3$ pb is given for $m = 0.3–1.7$ TeV.

³³ KHACHATRYAN 10 search for narrow dijet resonances in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 2.9$ pb⁻¹. Limits on the cross section in the range 1–300 pb is given for $m = 0.5–2.6$ TeV separately in the final states $qq, qg$, and $gg$.

³⁴ ABE 99f search for narrow $b\bar{b}$ resonances in $p\bar{p}$ collisions at $E_{cm} = 1.8$ TeV. Limits on $\sigma(p\bar{p} \to X + \text{anything}) \times B(X \to b\bar{b})$ in the range $3–10^3$ pb (95% CL) are given for $m_X = 200–750$ GeV. See their Table I.

³⁵ ABE 97G search for narrow dijet resonances in $p\bar{p}$ collisions with 106 pb⁻¹ of data at $E_{cm} = 1.8$ TeV. Limits on $\sigma(p\bar{p} \to X + \text{anything}) \times B(X \to jj)$ in the range $10^4–10^5$ pb (95% CL) are given for dijet mass $m = 200–1150$ GeV with both jets having $|\eta| < 2.0$ and the dijet system having $|\cos\theta'| < 0.67$. See their Table I for the list of limits. Supersedes ABE 93g.

³⁶ ABE 93g give cross section times branching ratio into light ($d, u, s, c, b$) quarks for $\Gamma = 0.02 M$. Their Table II gives limits for $M = 200–900$ GeV and $\Gamma = (0.02–0.2) M$.

## LIMITS ON NEUTRAL PARTICLE PRODUCTION

### Production Cross Section of Radiatively-Decaying Neutral Particle

<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;0.0008</td><td>95</td><td>1 ALBERT</td><td>18C HAWC</td><td>γ from Sun</td></tr><tr><td></td><td></td><td>2 KHACHATRYAN</td><td>17D CMS</td><td>Zγ resonance</td></tr><tr><td></td><td></td><td>3 AAD</td><td>16AI ATLS</td><td>pp → γ + jet</td></tr><tr><td></td><td></td><td>4 KHACHATRYAN</td><td>16M CMS</td><td>pp → γγ resonance</td></tr><tr><td>&lt;(0.043–0.17)</td><td>95</td><td>5 ABBIENDI</td><td>00D OPAL</td><td>e⁺e⁻ → X⁰Y⁰, X⁰ → Y⁰γ</td></tr><tr><td>&lt;(0.05–0.8)</td><td>95</td><td>6 ABBIENDI</td><td>00D OPAL</td><td>e⁺e⁻ → X⁰Y⁰, X⁰ → Y⁰γ</td></tr><tr><td>&lt;(2.5–0.5)</td><td>95</td><td>7 ACKERSTAFF</td><td>97B OPAL</td><td>e⁺e⁻ → X⁰Y⁰, X⁰ → Y⁰γ</td></tr><tr><td>&lt;(1.6–0.9)</td><td>95</td><td>8 ACKERSTAFF</td><td>97B OPAL</td><td>e⁺e⁻ → X⁰Y⁰, X⁰ → Y⁰γ</td></tr></tbody></table>

¹ ALBERT 18C search for WIMP annihilation in Sun to long-lived, radiatively decaying mediator; no signal; limits set on $\sigma^{SD}(\chi p)$ assuming long-lived mediator.

² KHACHATRYAN 17D search for new scalar resonance decaying to $Z\gamma$ with $Z \to e^+e^-$, $\mu^+\mu^-$ in $pp$ collisions at 8 and 13 TeV; no signal seen.

³ AAD 16AI search for excited quarks (EQ) and quantum black holes (QBH) in 3.2 fb⁻¹ at 13 TeV of data; exclude EQ below 4.4 TeV and QBH below 3.8 (6.2) TeV for RS1 (ADD) models. The visible cross section limit was obtained for 5 TeV resonance with $\sigma_G/M_G = 2\%$.

⁴ KHACHATRYAN 16M search for $\gamma\gamma$ resonance using 19.7 fb⁻¹ at 8 TeV and 3.3 fb⁻¹ at 13 TeV; slight excess at 750 GeV noted; limit set on RS graviton.

⁵ ABBIENDI 00d associated production limit is for $m_{X^0} = 90–188$ GeV, $m_{Y^0} = 0$ at $E_{cm} = 189$ GeV. See also their Fig. 9.

⁶ ABBIENDI 00d pair production limit is for $m_{X^0} = 45–94$ GeV, $m_{Y^0} = 0$ at $E_{cm} = 189$ GeV. See also their Fig. 12.

⁷ ACKERSTAFF 97B associated production limit is for $m_{X^0} = 80–160$ GeV, $m_{Y^0} = 0$ from 10.0 pb⁻¹ at $E_{cm} = 161$ GeV. See their Fig. 3(a).

⁸ ACKERSTAFF 97B pair production limit is for $m_{X^0} = 40–80$ GeV, $m_{Y^0} = 0$ from 10.0 pb⁻¹ at $E_{cm} = 161$ GeV. See their Fig. 3(b).

### Heavy Particle Production Cross Section

<table><thead><tr><th>VALUE (cm<sup>2</sup>/N)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td></td><td></td><td>1 AAD</td><td>23P ATLS</td><td>exotic search in association with h → γγ</td></tr><tr><td></td><td></td><td>2 TUMASYAN</td><td>23BC CMS</td><td>γ-jet resonance search</td></tr><tr><td></td><td></td><td>3 TUMASYAN</td><td>23BF CMS</td><td>pp + γ/Z + X search</td></tr><tr><td></td><td></td><td>4 TUMASYAN</td><td>22AG CMS</td><td>SIMP search</td></tr><tr><td></td><td></td><td>5 AAD</td><td>21F ATLS</td><td>monojet search</td></tr><tr><td></td><td></td><td>6 AAIJ</td><td>20AL LHCB</td><td>pp at 13 TeV, dimuon resonance</td></tr><tr><td></td><td></td><td>7 SIRUNYAN</td><td>20AY CMS</td><td>T(15) μ⁺μ⁻ decay states</td></tr><tr><td></td><td></td><td>8 SIRUNYAN</td><td>20Z CMS</td><td>multilepton BSM search, 13 TeV</td></tr><tr><td></td><td></td><td>9 AABOUD</td><td>19H ATLS</td><td>di-photon-jet resonance</td></tr><tr><td></td><td></td><td>10 AABOUD</td><td>19V ATLS</td><td>review, mediator-based DM</td></tr><tr><td></td><td></td><td>11 SIRUNYAN</td><td>19O CMS</td><td>pp → γ E<sub>T</sub></td></tr><tr><td></td><td></td><td>12 AABOUD</td><td>18CJ ATLS</td><td>pp → V/V/ℓℓ/ℓν, V = W, Z, h</td></tr><tr><td></td><td></td><td>13 AABOUD</td><td>18CM ATLS</td><td>pp → eμ/ετ/μτ</td></tr><tr><td></td><td></td><td>14 AAIJ</td><td>18AJ LHCB</td><td>pp → A' → μ⁺μ⁻; dark photon</td></tr><tr><td></td><td></td><td>15 BANERJEE</td><td>18 NA64</td><td>eZ → eZX(A')</td></tr><tr><td></td><td></td><td>16 BANERJEE</td><td>18A NA64</td><td>eZ → eZ A', A' → Xχ</td></tr><tr><td></td><td></td><td>17 MARSICANO</td><td>18 E137</td><td>e⁺e⁻ → A'(γ) visible decay</td></tr><tr><td></td><td></td><td>18 SIRUNYAN</td><td>18BB CMS</td><td>pp → Z' → ℓ⁺ℓ⁻ at 13 TeV</td></tr><tr><td></td><td></td><td>19 SIRUNYAN</td><td>18DA CMS</td><td>pp → Black Hole, string ball, sphaleron</td></tr><tr><td></td><td></td><td>20 SIRUNYAN</td><td>18DD CMS</td><td>pp → jj</td></tr><tr><td></td><td></td><td>21 SIRUNYAN</td><td>18DR CMS</td><td>pp → bμπ</td></tr><tr><td></td><td></td><td>22 SIRUNYAN</td><td>18DU CMS</td><td>pp → γγ</td></tr><tr><td></td><td></td><td>23 SIRUNYAN</td><td>18ED CMS</td><td>pp → V → Wh; h → b\bar{b}; W → ℓν</td></tr><tr><td></td><td></td><td>24 AABOUD</td><td>17B ATLS</td><td>WH, ZH resonance</td></tr><tr><td></td><td></td><td>25 AAIJ</td><td>17BR LHCB</td><td>pp → π<sub>V</sub> π<sub>V</sub>, π<sub>V</sub> → jj</td></tr><tr><td></td><td></td><td>26 AAD</td><td>16O ATLS</td><td>ℓ⁺ + (ℓs or jets)</td></tr><tr><td></td><td></td><td>27 AAD</td><td>16R ATLS</td><td>WW, WZ, ZZ resonance</td></tr><tr><td></td><td></td><td>28 KRASZNAHO</td><td>16E</td><td>p7Li → 8Be → X(17)N, X(17) → e⁺e⁻</td></tr><tr><td></td><td></td><td>29 LEES</td><td>15E BABR</td><td>e⁺e⁻ collisions</td></tr><tr><td></td><td></td><td>30 ADAMS</td><td>97B KTEV</td><td>m = 1.2–5 GeV</td></tr><tr><td></td><td></td><td>31 GALLAS</td><td>95 TOF</td><td>m = 0.5–20 GeV</td></tr><tr><td></td><td></td><td>32 AKESSON</td><td>91 CNTR</td><td>m = 0–5 GeV</td></tr><tr><td></td><td></td><td>33 BADIER</td><td>86 BDMP</td><td>τ = (0.05–1.) × 10⁻⁸ s</td></tr><tr><td></td><td></td><td>34 GUSTAFSON</td><td>76 CNTR</td><td>τ > 10⁻⁷ s</td></tr></tbody></table>

¹ AAD 23P search in 22 channels for exotica produced in association with $h \to \gamma\gamma$ in 139 fb⁻¹ of data. No signal observed. Limits placed on production cross section in various channels.
² TUMASYAN 23BC search for γ-jet resonance at CMS with 138 fb⁻¹ of data. No signal observed. Limits placed on quantum black hole and excited quark models.

³ TUMASYAN 23BF search for $pp \to pp + \gamma/Z + X$ search where X is missing particle using CMS-TOTEM with 37.2 fb⁻¹ of data. No signal observed. Limits placed on σ vs. m plane.

⁴ TUMASYAN 22AG search for strongly interacting neutral massive particles via trackless jets with 16.1 fb⁻¹ at 13 TeV; no signal detected; limits placed in mass vs. cross section plane for various simplified models.

⁵ AAD 21f search for hard monojet production at ATLAS with 139⁻¹ of 13 TeV data. No signal observed. Limits placed on invisible production cross-section recolliding against ISR and interpreted in variety of BSM models.

⁶ AAIJ 20AL search for dimuon resonance from promptly decaying X particle; no signal; limits placed on m(X) up to 60 GeV depending on mixing in 2HDM.

⁷ SIRUNYAN 20AY measured $\Upsilon(1S)\mu^+\mu^-$ at CMS with 13 TeV with 35.9 fb⁻¹. No signal is found and limits are set in σ. BF vs. mass plane for tetra-b-quarks with masses between 17.5 and 19 GeV and for generic search for narrow resonances with mass between 16.5 and 27 GeV.

⁸ SIRUNYAN 20Z search for BSM physics via multilepton production with CMS at 13 TeV with 137 fb⁻¹; no signal is found and limits are set on type-III seesaw and other BSM models.

⁹ AABOUD 19h searches for di-photon-jet resonance at 13 TeV and 36.7 fb⁻¹ of data; no signal found and limits placed on σ. BR vs. mass plane for various simplified models.

¹⁰ AABOUD 19v review ATLAS searches for mediator-based DM at 7, 8, and 13 TeV with up to 37 fb⁻¹ of data; no signal found and limits set for wide variety of simplified models of dark matter.

¹¹ SIRUNYAN 19o search for $pp \to \gamma E_T$ at 13 TeV with 36.1 fb⁻¹; no signal found and limits set for various simplified models.

¹² AABOUD 18CJ make multichannel search for $pp \to VV/\ell\ell/\ell\nu$, $V = W, Z, h$ at 13 TeV, 36.1 fb⁻¹; no signal found; limits placed for several BSM models.

¹³ AABOUD 18CM search for lepton-flavor violating resonance in $pp \to e\mu/e\tau/\mu\tau$ at 13 TeV, 36.1 fb⁻¹; no signal is found and limits placed for various BSM models.

¹⁴ AAIJ 18AJ search for prompt and delayed dark photon decay $A' \to \mu^+\mu^-$ at LHCb detector using 1.6 fb⁻¹ of $pp$ collisions at 13 TeV; limits on $m(A')$ vs. kinetic mixing are set.

¹⁵ BANERJEE 18 search for dark photon $A'/16.7$ MeV boson X at NA64 via $eZ \to eZX(A')$; no signal found and limits set on the $Xe^-e^-$ coupling $\epsilon_e$ in the range $1.3 \times 10^{-4} \le \epsilon_e \le 4.2 \times 10^{-4}$ excluding part of the allowed parameter space.

¹⁶ BANERJEE 18A search for invisibly decaying dark photons in $eZ \to eZA'$, $A' \to$ invisible; no signal found and limits set on mixing for $m(A') < 1$ GeV.

¹⁷ MARSICANO 18 search for dark photon $e^+e^- \to A'(\gamma)$ visible decay in SLAC E137 e beam dump data. No signal observed and limits set in $\epsilon$ coupling vs m(A') plane, see their figure 7.

¹⁸ SIRUNYAN 18BB search for high mass dilepton resonance; no signal found and exclude portions of p-space of $Z'$, KK graviton models.

¹⁹ SIRUNYAN 18DA search for $pp \to Black Hole, string ball, sphaleron via high multiplicity events at 13 TeV, 35.9 fb⁻¹; no signal, require e.g. m(BH) > 10.1 TeV.

²⁰ SIRUNYAN 18DD search for $pp \to jj$ deviations in dijet angular distribution. No signal observed. Set limits on large extra dimensions, black holes and DM mediators e.g. m(BH) > 5.9-8.2 TeV.

²¹ SIRUNYAN 18DR search for dimuon resonance in $pp \to b\mu\bar{\mu}$ at 8 and 13 TeV. Slight excess seen at $m(\mu\bar{\mu}) \sim 28$ GeV in some channels.

²² SIRUNYAN 18DU search for high mass diphoton resonance in $pp \to \gamma\gamma$ at 13 TeV using 35.9 fb⁻¹; no signal; limits placed on RS Graviton, LED, and clockwork.

²³ SIRUNYAN 18ED search for $pp \to V \to Wh; h \to b\bar{b}; W \to \ell\nu$ at 13 TeV with 35.9 fb⁻¹; no signal; limits set on $m(W') > 2.9$ TeV.

²⁴ AABOUD 17b exclude $m(W', Z') < 1.49-2.31$ TeV depending on the couplings and $W'/Z'$ degeneracy assumptions via WH, ZH search in $pp$ collisions at 13 TeV with 3.2 fb⁻¹ of data.

²⁵ AAIJ 17BR search for long-lived hidden valley pions from Higgs decay. Limits are set on the signal strength as a function of the mass and lifetime of the long-lived particle in their Fig. 4 and Tab. 4.

²⁶ AAD 160 search for $eH_T, \ell + (\ell s$ or jets) with 3.2 fb⁻¹ at 13 TeV; exclude micro black holes mass < 8 TeV (Fig. 3) for models with two extra dimensions.

²⁷ AAD 16R search for WW, WZ, ZZ resonance in 20.3 fb⁻¹ at 8 TeV data; limits placed on massive RS graviton (Fig. 4).

²⁸ KRASNAHORKAY 16 report $\text{PLi} \to e\bar{e}N 5\sigma$ resonance at 16.7 MeV—possible evidence for nuclear interference or new light boson. However, such nuclear interference was ruled out already by ZANG 17.

²⁹ LEES 15E search for long-lived neutral particles produced in $e^+e^-$ collisions in the Ursupin region, which decays into $e^+, \mu^+, \mu^-, \pm\mu^\mp, \pi^+, \pi^-, K^+, K^-, \text{or } \pi^\pm K^\pm$. See their Fig. 2 for cross section limits.

³⁰ ADAMS 97B search for a hadron-like neutral particle produced in $pN$ interactions, which decays into a $\rho^0$ and a weakly interacting massive particle. Upper limits are given for the ratio to $K_L$ production for the mass range 1.2-5 GeV and lifetime $10^{-9}-10^{-8}$ s. See also our Light Gluino Section.

³¹ GALLAS 95 limit is for a weakly interacting neutral particle produced in $pN$ interactions decaying with a lifetime of $10^{-4}-10^{-8}$ s. See their Figs. 8 and 9. Similar limits are obtained for a stable particle with interaction cross section $10^{-29}-10^{-33}$ cm². See Fig. 10.

³² AKESSON 91 limit is from weakly interacting neutral long-lived particles produced in $pN$ reaction at 450 GeV/c performed at CERN SPS. Bourguin-Gaillard formula is used as the production model. The above limit is for $\tau > 10^{-7}$ s. For $\tau > 10^{-9}$ s, $\sigma < 10^{-30}$ cm⁻²/nucleon is obtained.

³³ BADIER 86 looked for long-lived particles at 300 GeV $\pi^-$ beam dump. The limit applies for nonstrongly interacting neutral or charged particles with mass >2 GeV. The limit applies for particle modes, $\mu^+\pi^-, \mu^+\mu^-, \pi^+\pi^-X, \pi^+\pi^-\pi^\pm$ etc. See their figure 5 for the contours of limits in the mass-$\tau$ plane for each mode.

³⁴ GUSTAFSON 76 is a 300 GeV FNAL experiment looking for heavy ($m > 2$ GeV) long-lived neutral hadrons in the M4 neutral beam. The above typical value is for $m = 3$ GeV and assumes an interaction cross section of 1 mb. Values as a function of mass and interaction cross section are given in figure 2.

## Production of New Penetrating Non-ν Like States in Beam Dump

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td>We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1</td><td>ABRATENKO</td><td>22A</td><td>MCBN search for LLPs</td></tr><tr><td>2</td><td>ANDREEV</td><td>22A</td><td>NA64 search for new boson X in eZ → eZX</td></tr><tr><td>3</td><td>ANDREEV</td><td>21</td><td>NA64 search for new boson X in eZ → eZX</td></tr><tr><td>4</td><td>LOSECCO</td><td>81</td><td>CALO 28 GeV protons</td></tr></tbody></table>

¹ ABRATENKO 22a search for LLPs from kaon decay in MicroBooNE absorber; no signal observed; limits placed for heavy neutral leptons (HNLS) and Higgs portal scalars (HPSs) in the MeV mass range.

² ANDREEV 22a search for new light B-L gauge boson $Z' \to \nu\bar{\nu}$ in electron beam dump at NA64; no signal observed; limits set in $m(Z')$ vs coupling plane for $m(Z') \sim 10^{-6}-1$ GeV.

³ ANDREEV 21 search for new invisibly decaying boson X in $eZ \to eZX$ at NA64. No signal observed. Limits set in coupling vs. m(X) plane for m(X) $\sim 10^{-3}$ to 1 GeV.

⁴ No excess neutral-current events leads to $\sigma(\text{production}) \times \sigma(\text{interaction}) \times \text{acceptance} < 2.26 \times 10^{-71} \text{ cm}^4/\text{nucleon}^2$ (CL = 90%) for light neutrals. Acceptance depends on models (0.1 to 4. $\times 10^{-4}$).

## LIMITS ON CHARGED PARTICLES IN $e^+e^-$

### Heavy Particle Production Cross Section in $e^+e^-$

Ratio to $\sigma(e^+e^- \to \mu^+\mu^-)$ unless noted. See also entries in Free Quark Search and Magnetic Monopole Searches.

<table><thead><tr><th>VALUE</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td></td><td>We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1</td><td>ADACHI</td><td>23K</td><td>BELL search for LLP in B decays</td><td></td></tr><tr><td>2</td><td>KILE</td><td>18</td><td>Alep $e^+e^- \to 4$ jets</td><td></td></tr><tr><td>3</td><td>ABLIKIM</td><td>17AA</td><td>BES3 $e^+e^- \to \ell\bar{\ell}\gamma$</td><td></td></tr><tr><td>4</td><td>ACKERSTAFF</td><td>98P</td><td>OPAL Q=1,2/3, m=45-89.5 GeV</td><td></td></tr><tr><td>5</td><td>ABREU</td><td>97D</td><td>DLPH Q=1,2/3, m=45-84 GeV</td><td></td></tr><tr><td>6</td><td>BARATE</td><td>97K</td><td>Alep Q=1, m=45-85 GeV</td><td></td></tr><tr><td>7</td><td>AKERS</td><td>95R</td><td>OPAL Q=1, m=5-45 GeV</td><td></td></tr><tr><td>8</td><td>AKERS</td><td>95R</td><td>OPAL Q=2, m=5-45 GeV</td><td></td></tr><tr><td>9</td><td>BUSKULIC</td><td>93C</td><td>Alep Q=1, m=32-72 GeV</td><td></td></tr><tr><td>&lt;10<sup>-2</sup></td><td>95</td><td>ADACHI</td><td>90C TOPZ Q=1, m=1-16, 18-27 GeV</td><td></td></tr><tr><td>&lt;7<sup>-1</sup> × 10<sup>-2</sup></td><td>90</td><td>ADACHI</td><td>10 ADACHI 90E TOPZ Q=1, m=5-25 GeV</td><td></td></tr><tr><td>&lt;1.6<sup>-2</sup> × 10<sup>-2</sup></td><td>95</td><td>KINOSHITA</td><td>82 PLAS Q=3-180, m &lt;14.5 GeV</td><td></td></tr><tr><td>&lt;5.0<sup>-2</sup> × 10<sup>-2</sup></td><td>90</td><td>BARTEL</td><td>80 JADE Q=(3,4,5)/3 2-12 GeV</td><td></td></tr></tbody></table>

¹ ADACHI 23k search for spin-0 LLP called S in B decays. No signal observed. Limits placed in branching fraction vs. m(S) plane.

² KILE 18 investigate archived ALEPH $e^+e^- \to 4$ jets data and see 4-5 $\sigma$ excess at 110 GeV.

³ ABLIKIM 17AA search for dark photon A $\to \ell\bar{\ell}$ at 3.773 GeV with 2.93 fb⁻¹. Limits are set in $\epsilon$ vs m(A) plane.

⁴ ACKERSTAFF 98P search for pair production of long-lived charged particles at $E_{cm}$ between 130 and 183 GeV and give limits $\sigma < (0.05-0.2)$ pb (95%CL) for spin-0 and spin-1/2 particles with $m=45-89.5$ GeV, charge 1 and 2/3. The limit is translated to the cross section at $E_{cm}=183$ GeV with the $\sigma$ dependence described in the paper. See their Figs. 2-4.

⁵ ABREU 97D search for pair production of long-lived particles and give limits $\sigma < (0.4-2.3)$ pb (95%CL) for various center-of-mass energies $E_{cm}=130-136, 161$, and 172 GeV, assuming an almost flat production distribution in $\cos\beta$.

⁶ BARATE 97k search for pair production of long-lived charged particles at $E_{cm} = 130, 136, 161$, and 172 GeV and give limits $\sigma < (0.2-0.4)$ pb (95%CL) for spin-0 and spin-1/2 particles with $m=45-85$ GeV. The limit is translated to the cross section at $E_{cm}=172$ GeV with the $E_{cm}$ dependence described in the paper. See their Figs. 2 and 3 for limits on $J = 1/2$ and $J' = 0$ cases.

⁷ AKERS 95R is a CERN-LEP experiment with $W_{cm} \sim m_Z$. The limit is for the production of a stable particle in multihadron events normalized to $\sigma(e^+e^- \to \text{hadrons})$. Constant phase space distribution is assumed. See their Fig. 3 for bounds for $Q = \pm 2/3$, $\pm 4/3$.

⁸ BUSKULIC 93c is a CERN-LEP experiment with $W_{cm} = m_Z$. The limit is for a pair or single production of heavy particles with unusual ionization loss in TPC. See their Fig. 5 and Table 1.

⁹ ADACHI 90c is a KEK-TRISTAN experiment with $W_{cm} = 52-60$ GeV. The limit is for pair production of a scalar or spin-1/2 particle. See Figs. 3 and 4.

¹⁰ ADACHI 90e is KEK-TRISTAN experiment with $W_{cm} = 52-61.4$ GeV. Above limit is for inclusive production cross section normalized to $\sigma(e^+e^- \to \mu^+\mu^-)\beta(3-\beta^2)/2$, where $\beta = (1-4m^2/W_{cm}^2)^{1/2}$. See the paper for the assumption about the production mechanism.

¹¹ KINOSHITA 82 is SLAC PEP experiment at $W_{cm} = 29$ GeV using lexan and $^{39}$Cr plastic sheets sensitive to highly ionizing particles.

¹² BARTEL 80 is DESY-PETRA experiment with $W_{cm} = 27-35$ GeV. Above limit is for inclusive pair production and ranges between $1. \times 10^{-1}$ and $1. \times 10^{-2}$ depending on mass and production momentum distributions. (See their figures 9, 10, 11 and 12).

## Branching Fraction of $Z^0$ to a Pair of Stable Charged Heavy Fermions

<table><thead><tr><th>VALUE</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;5 × 10<sup>-6</sup></td><td>95</td><td>1 AKERS</td><td>95R</td><td>OPAL m = 40.4-45.6 GeV</td></tr><tr><td>&lt;1 × 10<sup>-3</sup></td><td>95</td><td>AKRAWY</td><td>900</td><td>OPAL m = 29-40 GeV</td></tr></tbody></table>

¹ AKERS 95R give the 95% CL limit $\sigma(X\bar{X})/\sigma(\mu\mu) < 1.8 \times 10^{-4}$ for the pair production of singly- or doubly-charged stable particles. The limit applies for the mass range 40.4-45.6 GeV for $X^\pm$ and $< 45.6$ GeV for $X^\pm\pm$. See the paper for bounds for $Q = \pm 2/3$, $\pm 4/3$.
## LIMITS ON CHARGED PARTICLES IN HADRONIC REACTIONS

### MASS LIMITS for Long-Lived Charged Heavy Fermions

Limits are for spin 1/2 particles with no color and SU(2)$_L$ charge. The electric charge $Q$ of the particle (in the unit of $e$) is therefore equal to its weak hypercharge. Pair production by Drell-Yan like $γ$ and $Z$ exchange is assumed to derive the limits.

VALUE (GeV) CL% DOCUMENT ID TECN COMMENT

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

<table><thead><tr><th></th><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td></td><td>1 AAD</td><td>23BT ATLS</td><td>multi-charged LLP</td><td></td></tr><tr><td></td><td>2 SIRUNYAN</td><td>20N CMS</td><td>disappearing track LLP</td><td></td></tr><tr><td>&gt;660</td><td>95</td><td>3 AAD</td><td>15BJ ATLS</td><td>|Q| = 2</td></tr><tr><td>&gt;200</td><td>95</td><td>4 CHATRCHYAN13AB CMS</td><td></td><td>|Q| = 1/3</td></tr><tr><td>&gt;480</td><td>95</td><td>4 CHATRCHYAN13AB CMS</td><td></td><td>|Q| = 2/3</td></tr><tr><td>&gt;574</td><td>95</td><td>4 CHATRCHYAN13AB CMS</td><td></td><td>|Q| = 1</td></tr><tr><td>&gt;685</td><td>95</td><td>4 CHATRCHYAN13AB CMS</td><td></td><td>|Q| = 2</td></tr><tr><td>&gt;140</td><td>95</td><td>5 CHATRCHYAN13AR CMS</td><td></td><td>|Q| = 1/3</td></tr><tr><td>&gt;310</td><td>95</td><td>5 CHATRCHYAN13AR CMS</td><td></td><td>|Q| = 2/3</td></tr></tbody></table>

1. AAD 23BT search for multi-charged long-lived particles with ATLAS detector using 139 fb⁻¹. No signal observed. Limits placed on LLP mass vs. charge plane.

2. SIRUNYAN 20N search for LLPs using disappearing track signature at CMS at 13 TeV with 101 fb⁻¹; no signal; limits placed on long-lived winos and higgsinos from SUSY depending on mass and lifetime: e.g. at 95% CL, for a purely higgsino neutralino, m(chargino) > 750 (175) GeV for $τ = 3$ (0.05) ns, and for a purely wino neutralino, m(chargino) > 884 (474) GeV for $τ = 3$ (0.2) ns.

3. AAD 15BJ use 20.3 fb⁻¹ of $pp$ collisions at $E_{cm} = 8$ TeV. See paper for limits for $|Q| = 3, 4, 5, 6$.

4. CHATRCHYAN 13AB use 5.0 fb⁻¹ of $pp$ collisions at $E_{cm} = 7$ TeV and 18.8 fb⁻¹ at $E_{cm} = 8$ TeV. See paper for limits for $|Q| = 3, 4, ..., 8$.

5. CHATRCHYAN 13AR use 5.0 fb⁻¹ of $pp$ collisions at $E_{cm} = 7$ TeV.

### Heavy Particle Production Cross Section

VALUE (nb) CL% DOCUMENT ID TECN COMMENT

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

<table><thead><tr><th></th><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td></td><td>1 AAD</td><td>24B ATLS</td><td>non-resonant jet search</td><td></td></tr><tr><td></td><td>2 AAD</td><td>22G ATLS</td><td>vector-like matter search</td><td></td></tr><tr><td></td><td>3 TUMASYAN</td><td>22H CMS</td><td>search for new matter via multileptons</td><td></td></tr><tr><td></td><td>4 SIRUNYAN</td><td>21T CMS</td><td>model independent search</td><td></td></tr><tr><td></td><td>5 SIRUNYAN</td><td>20C CMS</td><td>4t search via multileptons</td><td></td></tr><tr><td></td><td>6 AABOUD</td><td>19AA ATLS</td><td>BSM search</td><td></td></tr><tr><td></td><td>7 AABOUD</td><td>19Q ATLS</td><td>single top + MET</td><td></td></tr><tr><td></td><td>8 AABOUD</td><td>17D ATLS</td><td>anomalous WWjj, WZjj</td><td></td></tr><tr><td></td><td>9 AABOUD</td><td>17L ATLS</td><td>m&gt;870 GeV, Z(→ νν) tX</td><td></td></tr><tr><td>&lt;1.2 × 10⁻³</td><td>95</td><td>10 SIRUNYAN</td><td>17B CMS</td><td>tH</td></tr><tr><td>&lt;1.0 × 10⁻⁵</td><td>95</td><td>11 SIRUNYAN</td><td>17C CMS</td><td>Z + (t or b)</td></tr><tr><td>&lt;4.8 × 10⁻⁵</td><td>95</td><td>12 SIRUNYAN</td><td>17J CMS</td><td>X₅/₃ → tW</td></tr><tr><td>&lt;0.31–0.04 × 10⁻³</td><td>95</td><td>13 AAJ</td><td>15BD LHCB</td><td>m=124–309 GeV</td></tr><tr><td>&lt;0.19</td><td>95</td><td>14 AAD</td><td>13AH ATLS</td><td>|Q|=(2–6)e, m=50–600 GeV</td></tr><tr><td>&lt;1.0 × 10⁻⁵</td><td>95</td><td>15 AAD</td><td>11I ATLS</td><td>|Q| =10e, m=0.2–1 TeV</td></tr><tr><td>&lt;4.8 × 10⁻⁵</td><td>95</td><td>16.17 AALTONEN</td><td>09Z CDF</td><td>m&gt;100 GeV, noncolored</td></tr><tr><td>&lt;0.31–0.04 × 10⁻³</td><td>95</td><td>16.18 AALTONEN</td><td>09Z CDF</td><td>m&gt;100 GeV, colored</td></tr><tr><td>&lt;0.05</td><td>95</td><td>19 ABAZOV</td><td>09M D0</td><td>pair production</td></tr><tr><td>&lt;0.05</td><td>95</td><td>20 AKTAS</td><td>04C H1</td><td>m=3–10 GeV</td></tr><tr><td>&lt;0.30–130</td><td>95</td><td>21 ABE</td><td>92J CDF</td><td>m=50–200 GeV</td></tr><tr><td>&lt;100</td><td>95</td><td>22 CARROLL</td><td>78 SPEC</td><td>m=2–5 GeV</td></tr><tr><td></td><td></td><td>23 LEIPUNER</td><td>73 CNTR</td><td>m=3–11 GeV</td></tr></tbody></table>

1. AAD 24B search for non-resonant jets +MET at $\sqrt{s} = 13$ TeV with 139 fb⁻¹. No excess observed. Limits placed on EFT operators.

2. AAD 22G search for single vector-like quark $T$ with $T \to t\bar{t}$ in all hadronic mode with 139 fb⁻¹ at 13 TeV; no signal observed; limits placed in mass vs. coupling plane.

3. TUMASYAN 22H search for new states of matter via non-resonant muтивelopment production based on a luminosity of 138 fb⁻¹; no signal observed; limits placed on vector-like leptons, leptoquarks, and new fermions from type-III seesaw model.

4. SIRUNYAN 21T perform model unspecific search for deviations from SM with CMS at 13 TeV with 35.9⁻¹ fb data in numerous signature channels. No deviations from SM found.

5. SIRUNYAN 20C search for four top-quark production with decay to multileptons at CMS at 13 TeV with 137 fb⁻¹; no signal is found and limits are placed on the Higgs boson oblique parameter in the effective field theory framework (EFT) and the model parameters ($\tan\beta$).

6. AABOUD 19AA search for BSM physics at 13 TeV with 3.2 fb⁻¹ in > 10⁵ regions of > 700 event classes; no significant signal found.

7. AABOUD 19O search for single top+MET events at 13 TeV with 36.1 fb⁻¹ of data; no signal found and limits set in $\alpha$ or $\beta$ coupling vs. mass plane for variety of simplified models including DM and vector-like top quark $T$.

8. AABOUD 17D search for WWjj, WZjj in $pp$ collisions at 8 TeV with 3.2 fb⁻¹; set limits on anomalous couplings.

9. AABOUD 17L search for the pair production of heavy vector-like $T$ quarks in the $Z(→ \nu\nu) tX$ final state.

10. SIRUNYAN 17B search for vector-like quark $pp \to TX \to tHX$ in 2.3 fb⁻¹ at 13 TeV; no signal seen; limits placed.

11. SIRUNYAN 17C search for vector-like quark $pp \to TX \to Z + (t or b)$ in 2.3 fb⁻¹ at 13 TeV; no signal seen; limits placed.

12. SIRUNYAN 17J search for $pp \to X_5/3 X_5/3 \to tWtW$ with 2.3 fb⁻¹ at 13 TeV. No signal seen: $m(X) > 1020$ (990) GeV for RH (LH) new charge 5/3 quark.

13. AAJ 15BD search for production of long-lived particles in $pp$ collisions at $E_{cm} = 7$ and 8 TeV. See their Table 6 for cross section limits.

14. AAD 13AH search for production of long-lived particles with $|q|=(2–6)e$ in $pp$ collisions at $E_{cm} = 7$ TeV with 4.4 fb⁻¹. See their Fig. 8 for cross section limits.

15. AAD 11I search for production of highly ionizing massive particles in $pp$ collisions at $E_{cm} = 7$ TeV with $L = 3.1$ pb⁻¹. See their Table 5 for similar limits for $|q| = 6e$ and $17e$, Table 6 for limits on pair production cross section.

16. AALTONEN 09Z search for long-lived charged particles in $p\bar{p}T$ collisions at $E_{cm} = 1.96$ TeV with $L = 1.0$ fb⁻¹. The limits are on production cross section for a particle of mass above 100 GeV in the region $|\eta| \lesssim 0.7$, $p_T > 40$ GeV, and $0.4 < \beta < 1.0$.

17. Limit for weakly interacting charge-1 particle.

18. Limit for up-quark like particle.

19. ABAZOV 09M search for pair production of long-lived charged particles in $p\bar{p}$ collisions at $E_{cm} = 1.96$ TeV with $L = 1.1$ fb⁻¹. Limit on the cross section of (0.31–0.04) pb (95% CL) is given for the mass range of 60–300 GeV, assuming the kinematics of stau pair production.

20. AKTAS 04C look for charged particle photoproduction at HERA with mean c.m. energy of 200 GeV.

21. ABE 92J look for pair production of unit-charged particles which leave detector before decaying. Limit shown here is for $m=50$ GeV. See their Fig. 5 for different charges and stronger limits for higher mass.

22. CARROLL 78 look for neutral, $S = -2$ dihyperon resonance in $pp \to 2K^+X$. Cross section varies within above limits over mass range and $p_{lab} = 5.1–5.9$ GeV/c.

23. LEIPUNER 73 is an NAL 300 GeV $p$ experiment. Would have detected particles with lifetime greater than 200 ns.

### Heavy Particle Production Differential Cross Section

VALUE (cm²sr $^{-1}$ GeV⁻¹) CL% DOCUMENT ID TECN CHG COMMENT

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

<table><thead><tr><th></th><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td>&lt;2.6 × 10⁻³⁶</td><td>90</td><td>1 HAYRAPETY...23f CMS</td><td>top → $\ell$s via EFT ops.</td><td></td></tr><tr><td>&lt;2.2 × 10⁻³³</td><td>90</td><td>2 BALDIN 76 CNTR</td><td>$Q = 1, m=2.1–9.4 GeV$</td><td></td></tr><tr><td>&lt;1.1 × 10⁻³³</td><td>90</td><td>3 ALBROW 75 SPEC ±</td><td>$Q = \pm 1, m=4–15 GeV$</td><td></td></tr><tr><td>&lt;8. × 10⁻³⁵</td><td>90</td><td>3 ALBROW 75 SPEC ±</td><td>$Q = \pm 2, m=6–27 GeV$</td><td></td></tr><tr><td>&lt;1.5 × 10⁻³⁴</td><td>90</td><td>4 JOVANOV... 75 CNTR</td><td>$m=15–26 GeV$</td><td></td></tr><tr><td>&lt;6. × 10⁻³⁵</td><td>90</td><td>4 JOVANOV... 75 CNTR</td><td>$Q = \pm 2, m=3–10 GeV$</td><td></td></tr><tr><td>&lt;1. × 10⁻³¹</td><td>90</td><td>4 JOVANOV... 75 CNTR</td><td>$Q = \pm 2, m=10–26 GeV$</td><td></td></tr><tr><td>&lt;5.8 × 10⁻³⁴</td><td>90</td><td>5 APPEL 74 SPEC ±</td><td>$m=3.2–7.2 GeV$</td><td></td></tr><tr><td>&lt;1.2 × 10⁻³⁵</td><td>90</td><td>6 ALPER 73 SPEC ±</td><td>$m=1.5–24 GeV$</td><td></td></tr><tr><td>&lt;2.4 × 10⁻³⁵</td><td>90</td><td>7 ANTIPOV 71b CNTR</td><td>$Q = -, m=2.2–2.8$</td><td></td></tr><tr><td>&lt;2.4 × 10⁻³⁵</td><td>90</td><td>8 ANTIPOV 71c CNTR</td><td>$Q = -, m=1.2–1.7, 2.1–4$</td><td></td></tr><tr><td>&lt;1.5 × 10⁻³⁶</td><td>90</td><td>BINON 69 CNTR</td><td>$Q = -, m=1.1–8 GeV$</td><td></td></tr><tr><td>&lt;3.0 × 10⁻³⁶</td><td>90</td><td>9 DORFAN 65 CNTR</td><td>Be target $m=3–7$ GeV</td><td></td></tr><tr><td></td><td></td><td>9 DORFAN 65 CNTR</td><td>Fe target $m=3–7$ GeV</td><td></td></tr></tbody></table>

1. HAYRAPETYAN 23r search for anomalous top → leptons decay via effective operators. No signal observed. Limits placed on EFT operators.

2. BALDIN 76 is a 70 GeV Serpukhov experiment. Value is per Al nucleus at $\theta = 0$. For other charges in range $-0.5 \to -3.0$, CL = 90% limit is $(2.6 \times 10^{-36})/|(\text{charge})|$ for mass range $(2.1–9.4 \text{ GeV}) \times |(\text{charge})|$. Assumes stable particle interacting with matter as do antiprotons.

3. ALBROW 75 is a CERN ISR experiment with $E_{cm} = 53$ GeV, $\theta = 40$ mr. See figure 5 for mass ranges up to 35 GeV.

4. JOVANOVICH 75 is a CERN ISR 26+26 and 15+15 GeV $pp$ experiment. Figure 4 covers ranges $Q = 1/3$ to 2 and $m = 3$ to 26 GeV. Value is per GeV momentum.

5. APPEL 74 is NAL 300 GeV $pW$ experiment. Studies forward production of heavy (up to 24 GeV) charged particles with momenta 24–200 GeV (–charge) and 40–150 GeV (+charge). Above typical value is for 75 GeV and is per GeV momentum per nucleon.

6. ALPER 73 is CERN ISR 26+26 GeV $pp$ experiment. $p > 0.9$ GeV, $0.2 < \beta < 0.65$.

7. ANTIPOV 71b is from same 70 GeV $p$ experiment as ANTIPOV 71c and BINON 69.

8. ANTIPOV 71c limit inferred from flux ratio. 70 GeV $p$ experiment.

9. DORFAN 65 is a 30 GeV/c $p$ experiment at BNL. Units are per GeV momentum per nucleon.

### Long-Lived Heavy Particle Invariant Cross Section

VALUE (cm²/GeV²/N) CL% DOCUMENT ID TECN CHG COMMENT

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

<table><thead><tr><th></th><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td>&lt;5–700 × 10⁻³⁵</td><td>90</td><td>1 BERNSTEIN 88 CNTR</td><td></td><td></td></tr><tr><td>&lt;5–700 × 10⁻³⁷</td><td>90</td><td>1 BERNSTEIN 88 CNTR</td><td></td><td></td></tr><tr><td>&lt;2.5 × 10⁻³⁶</td><td>90</td><td>2 THRON 85 CNTR</td><td>$Q = 1, m=4–12 GeV$</td><td></td></tr><tr><td>&lt;1. × 10⁻³⁵</td><td>90</td><td>2 THRON 85 CNTR</td><td>$Q = 1, m=4–12 GeV$</td><td></td></tr><tr><td>&lt;6. × 10⁻³³</td><td>90</td><td>3 ARMITAGE 79 SPEC</td><td>$m=1.87$ GeV</td><td></td></tr><tr><td>&lt;1.5 × 10⁻³³</td><td>90</td><td>3 ARMITAGE 79 SPEC</td><td>$m=1.5–3.0 GeV$</td><td></td></tr><tr><td>&lt;1.1 × 10⁻³⁷</td><td>90</td><td>4 BOZZOLI 79 CNTR</td><td>$Q = (2/3, 1/4, 3/2)$</td><td></td></tr><tr><td>&lt;3.0 × 10⁻³⁷</td><td>90</td><td>5 CUTTS 78 CNTR</td><td>$m=4–10$ GeV</td><td></td></tr><tr><td></td><td></td><td>6 VIDAL 78 CNTR</td><td>$m=4.5–6$ GeV</td><td></td></tr></tbody></table>

1. BERNSTEIN 88 limits apply at $x = 0.2$ and $p_T = 0$. Mass and lifetime dependence of limits are shown in the regions: $m = 1.5–7.5$ GeV and $\tau = 10^{-8}–2 \times 10^{-6}$ s. First number is for hadrons; second is for weakly interacting particles.

2. THRON 85 is FNAL 400 GeV proton experiment. Mass determined from measured velocity and momentum. Limits are for $\tau > 3 \times 10^{-9}$ s.

3. ARMITAGE 79 is CERN-ISR experiment at $E_{cm} = 53$ GeV. Value is for $x = 0.1$ and $p_T = 0.15$. Observed particles at $m = 1.87$ GeV are found all consistent with being antideuteronics.

4. BOZZOLI 79 is CERN-SPS 200 GeV $pN$ experiment. Looks for particle with $\tau$ larger than $10^{-8}$ s. See their figure 11–18 for production cross-section upper limits vs mass.

5. CUTTS 78 is $p$Be experiment at FNAL sensitive to particles of $\tau > 5 \times 10^{-8}$ s. Value is for $-0.3 < x < 0$ and $p_T = 0.175$.

6. VIDAL 78 is FNAL 400 GeV proton experiment. Value is for $x = 0$ and $p_T = 0$. Puts lifetime limit of $< 5 \times 10^{-8}$ s on particle in this mass range.
Long-Lived Heavy Particle Production
($\sigma$(Heavy Particle) / $\sigma(\pi)$)

VALUE EVTS DOCUMENT_ID TECN CHG COMMENT

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

<table><tr><td>&lt;10<sup>-8</sup></td><td>1</td><td>NAKAMURA</td><td>89</td><td>SPEC ±</td><td>Q = (-5/3,±2)</td></tr><tr><td></td><td>0</td><td>BUSSIERE</td><td>80</td><td>CNTR ±</td><td>Q = (2/3,1/4,3/2)</td></tr></table>

¹NAKAMURA 89 is KEK experiment with 12 GeV protons on Pt target. The limit applies for mass ≲ 1.6 GeV and lifetime ≳ 10⁻⁷ s.

²BUSSIERE 80 is CERN-SPS experiment with 200–240 GeV protons on Be and Al target. See their figures 6 and 7 for cross-section ratio vs mass.

Production and Capture of Long-Lived Massive Particles

VALUE (10⁻³⁶ cm²) DOCUMENT_ID TECN COMMENT

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

<table><tr><td></td><td>1 AAD</td><td>21x ATLS</td><td>search for captured LLPs</td></tr><tr><td></td><td>2 ACHARYA</td><td>21 INDU</td><td>dyons production, capture</td></tr><tr><td>&lt;20 to 800</td><td>3 ALEKSEEV</td><td>76 ELEC</td><td>τ=5 ms to 1 day</td></tr><tr><td>&lt;200 to 2000</td><td>3 ALEKSEEV</td><td>76B ELEC</td><td>τ=100 ms to 1 day</td></tr><tr><td>&lt;1.4 to 9</td><td>4 FRANKEL</td><td>75 CNTR</td><td>τ=50 ms to 10 hours</td></tr><tr><td>&lt;0.1 to 9</td><td>5 FRANKEL</td><td>74 CNTR</td><td>τ=1 to 1000 hours</td></tr></table>

¹AAD 21x search for LLPs which come to rest in ATLAS detector to deposit energy between collisions. No signal observed in 111 fb⁻¹ of data. Limits placed in lifetime vs. mass place assuming model with gluino hadrons: e.g. m > 1.4 TeV for τ ~ 10⁻⁵ to 10³ sec.

²ACHARYA 21 search for dyons (carrying electric and magnetic charge) and monopoles via production and capture in 6.46 fb⁻¹ of 13 TeV LHC data. No signal observed. Limits placed in mass vs. magnetic charge plane.

³ALEKSEEV 76 and ALEKSEEV 76b are 61–70 GeV p Serpukhov experiment. Cross section is per Pb nucleus.

⁴FRANKEL 75 is extension of FRANKEL 74.

⁵FRANKEL 74 looks for particles produced in thick Al targets by 300–400 GeV/c protons.

Long-Lived Particle (LLP) Search at Hadron Collisions

Limits are for cross section times branching ratio.

VALUE (fb) CL% DOCUMENT_ID TECN COMMENT

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

<table><tr><td></td><td>1 AAD</td><td>23AM ATLS</td><td>LLP higgsino search</td></tr><tr><td></td><td>2 AAD</td><td>23AR ATLS</td><td>LLP search via displaced γ</td></tr><tr><td></td><td>3 AAD</td><td>23BQ ATLS</td><td>displaced dimuon search</td></tr><tr><td></td><td>4 AAD</td><td>23CO ATLS</td><td>highly ionizing LLP/monopole</td></tr><tr><td></td><td>5 AAD</td><td>23G ATLS</td><td>heavy highly ionizing LLP search</td></tr><tr><td></td><td>6 AAD</td><td>23I ATLS</td><td>light LLP via collimated decays</td></tr><tr><td></td><td>7 TUMASYAN</td><td>23AO CMS</td><td>LLP search via trackless jets</td></tr><tr><td></td><td>8 TUMASYAN</td><td>23G CMS</td><td>LLP search via displaced dimuons</td></tr><tr><td></td><td>9 AAD</td><td>22H ATLS</td><td>LLP search with μ spectrometer</td></tr><tr><td></td><td>10 AAD</td><td>22K ATLS</td><td>LLP search via displaced jets in the calorimeter</td></tr><tr><td></td><td>11 AAD</td><td>22U ATLS</td><td>LLP/chargino search via tracklet</td></tr><tr><td></td><td>12 AAIJ</td><td>22U LHCB</td><td>LLP semileptonic decay to muon</td></tr><tr><td></td><td>13 ACHARYA</td><td>22A MOED</td><td>monopoles/HECOs at LHC</td></tr><tr><td></td><td>14 TUMASYAN</td><td>22AD CMS</td><td>heavy neutral lepton LLP search</td></tr><tr><td></td><td>15 TUMASYAN</td><td>22AF CMS</td><td>LLP search via displaced lepton tracks</td></tr><tr><td></td><td>16 TUMASYAN</td><td>22M CMS</td><td>LLP search via ZH production</td></tr><tr><td></td><td>17 TUMASYAN</td><td>22N CMS</td><td>LLP search via dimuons</td></tr><tr><td></td><td>18 AAD</td><td>21AL ATLS</td><td>charged LLPs search</td></tr><tr><td></td><td>19 AAD</td><td>21BA ATLS</td><td>LLP from higgs decay search</td></tr><tr><td></td><td>20 AAIJ</td><td>21V LHCB</td><td>LLP → eμν search</td></tr><tr><td></td><td>21 SIRUNYAN</td><td>21AF CMS</td><td>LLP search via displaced jets</td></tr><tr><td></td><td>22 SIRUNYAN</td><td>21U CMS</td><td>LLP search via displaced jets</td></tr><tr><td></td><td>23 TUMASYAN</td><td>21 CMS</td><td>LLP endcap muon detector searches</td></tr><tr><td></td><td>24 AAD</td><td>20D ATLS</td><td>pp → LLPs at 13 TeV</td></tr><tr><td></td><td>25 AAD</td><td>20J ATLS</td><td>scalar boson decay to LLPs</td></tr><tr><td></td><td>26 AAD</td><td>20M ATLS</td><td>LLP top squark decay to μ</td></tr><tr><td></td><td>27 AAD</td><td>20P ATLS</td><td>LLP dark photon search</td></tr><tr><td></td><td>28 AAIJ</td><td>20AL LHCB</td><td>pp dimuon resonance</td></tr><tr><td></td><td>29 BALL</td><td>20</td><td>LLP multi-charged particles at LHC</td></tr><tr><td></td><td>30 AABOUD</td><td>19AE ATLS</td><td>pp at 13 TeV</td></tr><tr><td></td><td>31 AABOUD</td><td>19AK ATLS</td><td>pp → Φ → ZZd</td></tr><tr><td></td><td>32 AABOUD</td><td>19AM ATLS</td><td>DY multi-charged LLP production</td></tr><tr><td></td><td>33 AABOUD</td><td>19AO ATLS</td><td>LLP via displaced jets</td></tr><tr><td></td><td>34 AABOUD</td><td>19AT ATLS</td><td>heavy, charged LLPs</td></tr><tr><td></td><td>35 AABOUD</td><td>19G ATLS</td><td>LLP decay to μ⁺μ⁻</td></tr><tr><td></td><td>36 SIRUNYAN</td><td>19BH CMS</td><td>LLP via displaced jets</td></tr><tr><td></td><td>37 SIRUNYAN</td><td>19BT CMS</td><td>LLP via displaced jets+MET</td></tr><tr><td></td><td>38 SIRUNYAN</td><td>19CA CMS</td><td>LLP → γ search</td></tr><tr><td></td><td>39 SIRUNYAN</td><td>19Q CMS</td><td>pp → j + displaced dark quark jet</td></tr><tr><td></td><td>40 SIRUNYAN</td><td>18AW CMS</td><td>Long-lived particle search</td></tr><tr><td></td><td>41 AAIJ</td><td>16AR LHCB</td><td>H → XX LLPs</td></tr><tr><td></td><td>42 KHACHATRY...16BWCMS</td><td></td><td>direct production: HSCPs</td></tr><tr><td></td><td>43 BADIER</td><td>86 BDMP</td><td>τ = (0.05–1.) × 10⁻⁸s</td></tr></table>

¹AAD 23AM search for long-lived higgsinos from gauge-mediation which decay to Z or H. No signal observed. Limits placed in cτ vs m(χ) plane for various simplified models.

²AAD 23AR search for long-lived particles via decay to displaced γ with 139 fb⁻¹ of data. No signal observed. Limits placed in m vs. τ and BF vs. τ planes for gauge-mediated SUSY model.

³AAD 23BQ search for displaced dimuon events in ATLAS detector. No signal observed. Limits placed in smuon lifetime vs. mass plane for long-lived smuon model.

⁴AAD 23CO search for monopoles and high-electric-charge LLPs in ATLAS with 139 fb⁻¹ of data. No signal observed. Limits placed in mass vs. charge plane.

⁵AAD 23G search for heavy highly ionizing long-lived particles with 139 fb⁻¹ of data. No signal observed. Limits placed in m vs. τ plane for several SUSY models.

⁶AAD 23I search for light long-lived particles decaying to collimated decay products (e.g. dileptons). No signal observed. Limits placed in BF vs. τ plane.

⁷TUMASYAN 23AO search for trackless jets from LLP production at CMS. No signal observed. Limits placed for SUSY model with long-lived neutralino in m(χ) vs. cτ plane.

⁸TUMASYAN 23G search for LLP decaying to displaced dimuons at CM with 97.6 fb⁻¹ fb of data. No signal observed. Limits placed in cτ vs. m plane for hidden Abelian Higgs simplified model.

⁹AAD 22H search for scalar mediator decay to two LLPs which decay in muon chambers with 139 fb⁻¹ at 13 TeV; no signal detected; limits placed on various simplified models.

¹⁰AAD 22K search for LLP pair production via scalar mediator with LLP decay in hadron calorimeter; no signal detected; limits placed for various simplified models.

¹¹AAD 22U search for chargino LLP via disappearing tracks; no signal observed; limits placed in m(chargino) vs lifetime plane for cases of higgsino- or wino-like chargino.

¹²AAIJ 22U reports search for LLP production at LHCB with 5.4 fb⁻¹ at 13 TeV followed by semileptonic decay to muon; no signal detected; limits placed in mass or lifetime vs. cross section plane for several simplified models.

¹³ACHARYA 22A report search for monopole and HECO production via DY at 8 TeV LHC with 2.2 fb⁻¹ with MoEDAL detector; no signal detected; limits placed in mass vs. cross section plane for various electric/magnetic charge scenarios.

¹⁴TUMASYAN 22AD search for heavy neutral lepton which decays as LLP to trilepton state with 138 fb⁻¹ at 13 TeV; no signal detected; limits placed in mass vs. coupling plane.

¹⁵TUMASYAN 22AF search for LLPs via displaced lepton vertices. The analysis is performed with an integrated luminosity of 118 (113) fb⁻¹ when analyzing the ee (eμ, μμ) channel; no signal detected; limits placed for a variety of simplified models.

¹⁶TUMASYAN 22M search in 117 fb⁻¹ of 13 TeV data for ZH production with H → SS where S is a LLP; no signal observed; limits placed in decay length vs. branching fraction plane.

¹⁷TUMASYAN 22N search in 101 fb⁻¹ of 13 TeV data for LLP production via decay to dimuons; no signal observed; limits placed on mass vs. coupling or lifetime for a variety of simplified models.

¹⁸AAD 21AL reports on ATLAS search for long-lived charged particles with 139 fb⁻¹ at 13 TeV. No signal observed. Limits placed in lifetime vs. mass plane: e.g. for τ(LLP) ~ 0.1 ns, m选 electron) > 720 GeV.

¹⁹AAD 21BA search for long-lived particles from ZH production (H → b ¯b) with 2 displaced vertices in 139 fb⁻¹ of data at 13 TeV. No signal detected. Limits placed in branching fraction vs. lifetime plane.

²⁰AAIJ 21V search for pp → LLP + LLP with LLP → eμν in the lifetime range between 2 and 50 ps at LHCb with 5.4 fb⁻¹ at 13 TeV. No signal observed. Limits placed in LLP cross section vs. mass or lifetime plane for m(LLP) ~ 7 to 50 GeV.

²¹SIRUNYAN 21AF search for LLPs at CMS via jets with 2 displaced vertices in 140 fb⁻¹ of data at 13 TeV. No signal observed. Limits placed for RPV SUSY models in which a long-lived neutralino or gluino decays into a multijet final state with top, bottom, and strange quarks.

²²SIRUNYAN 21U search for long-lived particles (LLPs) via displaced jets at CMS with LHC13 and 132 fb⁻¹. No signal detected. Limits placed on simplified model production of LLP X → q ¯q with σ < 0.07 fb for m(X) > 500 GeV and cτ ~ 2 to 250 mm.

²³TUMASYAN 21 search for long-lived particles in CMS muon endcap detector in 137 fb⁻¹ of data at 13 TeV. No signal detected. Limits are placed depending on the branching fraction of Higgs boson to LLP decaying to dd, b ¯b, and τ⁺τ⁻, depending on proper decay length, and LLP masses.

²⁴AAD 20D search for opposite-sign dileptons originating from long-lived particles in pp collisions at 13 TeV with 32.8 fb⁻¹; limits placed in squark cross section vs. cτ plane for RPV SUSY.

²⁵AAD 20J search for scalar boson decay to two long-lived particles; no signal; limits placed in BF vs cτ plane for various mass hypotheses. This search is also combined with other ATLAS displaced-jet searches.

²⁶AAD 20M search for long-lived top-squarks decay to μ and hadrons; no signal; limits placed in cross section vs. mass and mass vs. lifetime planes.

²⁷AAD 20P search for long-lived dark photons produced from the decay of a scalar boson, with each dark photon decaying into displaced collimated leptons or light hadrons at 13 TeV with 36 fb⁻¹; no signal; limits placed in σ · BF vs. cτ and other planes.

²⁸AAIJ 20AL search for long-lived X → μ⁺μ⁻ decays in 5.1 fb⁻¹ of LHCb data at 13 TeV; no signal; limits placed on m(X) up to 3 GeV depending on kinetic mixing.

²⁹BALL 20 search for long-lived milli-charged particles produced at LHC; limits placed in charge vs. mass plane (Fig. 8).

³⁰AABOUD 19AE search for long-lived particles via displaced jets using 10.8 fb⁻¹ or 33.0 fb⁻¹ data (depending on a trigger) at 13 TeV; no signal found and limits set in branching ratio vs. decay length plane.

³¹AABOUD 19AK searches for long-lived particle Zd via pp → Φ → ZZd at 13 TeV with 36.1 fb⁻¹; no signal found and limits set in σ · BR vs. lifetime plane for simplified model.

³²AABOUD 19AM search for Drell-Yan (DY) production of long-lived multi-charge particles at 13 TeV with 36.1 fb⁻¹ of data; no signal found and exclude 50 GeV < m(LLMCP) < 980–1220 GeV for electric charge |q| = (2–7).

³³AABOUD 19AO search for neutral long-lived particles producing displaced jets at 13 TeV with 36.1 fb⁻¹ of data; no signal found and exclude regions of σ · BR vs. lifetime plane for various models.

³⁴AABOUD 19AT search for heavy, charged long-lived particles at 13 TeV with 36.1 fb⁻¹; no signal found and upper limits set on masses of various hypothetical particles.

³⁵AABOUD 9D search for long-lived particle with decay to μ⁺μ⁻ at 13 TeV with 32.9 fb⁻¹; no signal found and limits set in combinations of lifetime, mass and coupling planes for various simplified models.

³⁶SIRUNYAN 19BH search for long-lived SUSY particles via displaced jets at 13 TeV with 35.9 fb⁻¹; no signal found and limits placed in mass vs lifetime plane for various hypothetical models.
# Searches Particle Listings

## Other Particle Searches

³⁷ SIRUNYAN 19BT search for displaced jet(s)+E_T at 13 TeV with 137 fb⁻¹; no signal found and limits placed in mass vs lifetime plane for gauge mediated SUSY breaking models.

³⁸ SIRUNYAN 19CA search for gluino/squark decay to long-lived neutralino, decay to γ in GMSB; no signal, limits placed in m(χ) vs. lifetime plane for SPS8 GMSB benchmark point.

³⁹ SIRUNYAN 19O search for pp → j + displaced jet via dark quark with 13 TeV at 16.1 fb⁻¹; no signal found and limits set in mass vs lifetime plane for dark quark/dark pion model.

⁴⁰ SIRUNYAN 18AW search for very long lived particles (LLPs) decaying hadronically or to μπ in CMS detector; none seen/limits set on lifetime vs. cross section.

⁴¹ AAIJ 16AR search for long lived particles from H → XX with displaced X decay vertex using 0.62 fb⁻¹ at 7 TeV; limits set in Fig. 7.

⁴² KHACHATRYAN 16BW search for heavy stable charged particles via ToF with 2.5 fb⁻¹ at 13 TeV; require stable m(gluino/ball) > 1610 GeV.

⁴³ BADIER 86 looked for long-lived particles at 300 GeV π⁻ beam dump. The limit applies for nonstrongly interacting neutral or charged particles with mass >2 GeV. The limit applies for particle modes, μ⁺π⁻, μ⁺μ⁻, π⁺π⁻X, π⁺π⁻π∓ etc. See their figure 5 for the contours of limits in the mass-τ plane for each mode.

## Long-Lived Heavy Particle Cross Section

<table><thead><tr><th>VALUE (pb/sr)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;34</td><td>95</td><td>¹RAM</td><td>94</td><td>SPEC 1015&lt;m<sub>X++</sub> &lt;1085 MeV</td></tr><tr><td>&lt;75</td><td>95</td><td>¹RAM</td><td>94</td><td>SPEC 920&lt;m<sub>X++</sub> &gt;1025 MeV</td></tr></tbody></table>

¹ RAM 94 search for a long-lived doubly-charged fermion $X^{++}$ with mass between $m_N$ and $m_N+m_π$ and baryon number +1 in the reaction $pp \to X^{++}n$. No candidate is found. The limit is for the cross section at 15° scattering angle at 460 MeV incident energy and applies for $τ(X^{++}) \gg 0.1$ µs.

## LIMITS ON CHARGED PARTICLES IN COSMIC RAYS

### Heavy Particle Flux in Cosmic Rays

<table><thead><tr><th>VALUE (cm<sup>-2</sup>γr<sup>-1</sup>)</th><th>CL%</th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 6.2 &times; 10<sup>-10</sup></td><td>90</td><td>0</td><td>1 ALEMANNO</td><td>22</td><td>DAMP fractionally charged particles in space</td></tr><tr><td></td><td></td><td></td><td>2 CAO</td><td>22</td><td>superheavy DM &rarr; γ rays</td></tr><tr><td></td><td></td><td></td><td>3 ALVIS</td><td>18</td><td>MAJD Fractionally charged</td></tr><tr><td>&lt; 1 &times; 10<sup>-8</sup></td><td>90</td><td></td><td>4 AGNESE</td><td>15</td><td>CDM2 Q = 1/6</td></tr><tr><td>~ 6 &times; 10<sup>-9</sup></td><td></td><td>2</td><td>5 SAITO</td><td>90</td><td>Q &asymp; 14, m &asymp; 370m<sub>p</sub></td></tr><tr><td>&lt; 1.4 &times; 10<sup>-12</sup></td><td>90</td><td>0</td><td>6 MINCER</td><td>85</td><td>CALO m &ge; 1 TeV</td></tr><tr><td></td><td></td><td></td><td>7 SAKUYAMA</td><td>83B</td><td>PLAS m &sim; 1 TeV</td></tr><tr><td>&lt; 1.7 &times; 10<sup>-11</sup></td><td>99</td><td>0</td><td>8 BHAT</td><td>82</td><td>CC</td></tr><tr><td>&lt; 1 &times; 10<sup>-9</sup></td><td>90</td><td>0</td><td>9 MARINI</td><td>82</td><td>CNTR Q = 1, m &asymp; 4.5m<sub>p</sub></td></tr><tr><td>2 &times; 10<sup>-9</sup></td><td></td><td>3</td><td>10 YOCK</td><td>81</td><td>SPRK Q = 1, m &asymp; 4.5m<sub>p</sub></td></tr><tr><td></td><td></td><td></td><td>10 YOCK</td><td>81</td><td>SPRK Fractionally charged</td></tr><tr><td>3.0 &times; 10<sup>-9</sup></td><td></td><td>3</td><td>11 YOCK</td><td>80</td><td>SPRK m &asymp; 4.5 m<sub>p</sub></td></tr><tr><td>(4 &plusmn;1) &times; 10<sup>-11</sup></td><td></td><td>3</td><td>GOODMAN</td><td>79</td><td>ELEC m &ge; 5 GeV</td></tr><tr><td>&lt; 1.3 &times; 10<sup>-9</sup></td><td>90</td><td></td><td>12 BHAT</td><td>78</td><td>CNTR m &gt;1 GeV</td></tr><tr><td>&lt; 1.0 &times; 10<sup>-9</sup></td><td></td><td>0</td><td>BRIATORE</td><td>76</td><td>ELEC</td></tr><tr><td>&lt; 7. &times; 10<sup>-10</sup></td><td>90</td><td>0</td><td>YOCK</td><td>75</td><td>ELEC Q &gt;7e or &lt; -7e</td></tr><tr><td>&gt; 6. &times; 10<sup>-9</sup></td><td></td><td>0</td><td>13 YOCK</td><td>74</td><td>CNTR m &gt;6 GeV</td></tr><tr><td>&lt; 3.0 &times; 10<sup>-8</sup></td><td></td><td>5</td><td>DARDO</td><td>72</td><td>CNTR</td></tr><tr><td>&lt; 1.5 &times; 10<sup>-9</sup></td><td></td><td>0</td><td>TONWAR</td><td>72</td><td>CNTR m &gt;10 GeV</td></tr><tr><td>&lt; 3.0 &times; 10<sup>-10</sup></td><td></td><td>0</td><td>BJORNBOE</td><td>68</td><td>CNTR m &gt;5 GeV</td></tr><tr><td>&lt; 5.0 &times; 10<sup>-11</sup></td><td>90</td><td>0</td><td>JONES</td><td>67</td><td>ELEC m=5-15 GeV</td></tr></tbody></table>

¹ ALEMANNO 22 search for flux of fractionally charged particles (FCPs) in space; no signal observed; limits set in flux vs charge plane for mass as low as GeV.

² CAO 22 search for superheavy DM decaying to gamma rays; no signal observed; limits placed in mass vs. lifetime plane for m ~ 10⁵⁻¹⁰⁹ GeV for DM decays to bD or τπ.

³ ALVIS 18 search for fractional charged flux of cosmic matter at Majorana demonstrator; no signal observed and limits are set on the flux of lightly ionizing particles for charge as low as e/1000.

⁴ See AGNESE 15 Fig. 6 for limits extending down to Q = 1/200.

⁵ SAITO 90 candidates carry about 450 MeV/nucleon. Cannot be accounted for by conventional backgrounds. Consistent with strange quark matter hypothesis.

⁶ MINCER 85 is high statistics study of calorimeter signals delayed by 20–200 ns. Calibration with AGS beam shows they can be accounted for by rare fluctuations in signals from low-energy hadrons in the shower. Claim that previous delayed signals including BJORNBOE 68, DARDO 72, BHAT 82, SAKUYAMA 83b below may be due to this fake effect.

⁷ SAKUYAMA 83b analyzed 6000 extended air shower events. Increase of delayed particles and change of lateral distribution above 10¹⁷ eV may indicate production of very heavy parent at top of atmosphere.

⁸ BHAT 82 observed 12 events with delay > 2. × 10⁻⁸ s and with more than 40 particles. 1 eV has good hadron shower. However all events are delayed in only one of two detectors in cloud chamber, and could not be due to strongly interacting massive particle.

⁹ MARINI 82 applied PEP-counter for TOF. Above limit is for velocity = 0.54 of light. Limit is inconsistent with YOCK 80 YOCK 81 events if isotropic dependence on zenith angle is assumed.

¹⁰ YOCK 81 saw another 3 events with Q = ±1 and m about 4.5m_p as well as 2 events with m >5.3m_p, Q = ±0.75 ± 0.05 and m >2.8m_p, Q = ±0.70 ± 0.05 and 1 event with m = (9.3 ± 3)m_p, Q = ±0.89 ± 0.06 as possible heavy candidates.

¹¹ YOCK 80 events are with charge exactly or approximately equal to unity.

¹² BHAT 78 is at Kolar gold fields. Limit is for τ > 10⁻⁶ s.

¹³ YOCK 74 events could be tritons.

## Superheavy Particle (Quark Matter) Flux in Cosmic Rays

<table><thead><tr><th>VALUE<br>(cm<sup>-2</sup>γr<sup>-1</sup>)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;5 × 10<sup>-16</sup></td><td>90</td><td>1 ADRIANI</td><td>15</td><td>PMLA 4 &lt; m &lt; 1.2 × 10<sup>5</sup> m<sub>p</sub></td></tr><tr><td>&lt;1.8 × 10<sup>-12</sup></td><td>90</td><td>2 AMBROSIO</td><td>00b</td><td>MCPRO m &gt; 5 × 10<sup>14</sup> GeV</td></tr><tr><td>&lt;1.1 × 10<sup>-14</sup></td><td>90</td><td>3 ASTONE</td><td>93</td><td>CNTR m ≥ 1.5 × 10<sup>-13</sup> gram</td></tr><tr><td>&lt;2.2 × 10<sup>-14</sup></td><td>90</td><td>4 AHLEN</td><td>92</td><td>MCPRO 10<sup>-10</sup> &lt; m &lt; 0.1 gram</td></tr><tr><td>&lt;6.4 × 10<sup>-16</sup></td><td>90</td><td>5 NAKAMURA</td><td>91</td><td>PLAS m &gt; 10<sup>11</sup> GeV</td></tr><tr><td>&lt;2.0 × 10<sup>-11</sup></td><td>90</td><td>6 ORITO</td><td>91</td><td>PLAS m &gt; 10<sup>12</sup> GeV</td></tr><tr><td>&lt;4.7 × 10<sup>-12</sup></td><td>90</td><td>7 LIU</td><td>88</td><td>BOLO m &gt; 1.5 × 10<sup>-13</sup> gram</td></tr><tr><td>&lt;3.2 × 10<sup>-11</sup></td><td>90</td><td>8 BARISH</td><td>87</td><td>CNTR 1.4 × 10<sup>8</sup> &lt; m &lt; 10<sup>12</sup> GeV</td></tr><tr><td>&lt;3.5 × 10<sup>-11</sup></td><td>90</td><td>9 NAKAMURA</td><td>85</td><td>CNTR m &gt; 1.5 × 10<sup>-13</sup> gram</td></tr><tr><td>&lt;7. × 10<sup>-11</sup></td><td>90</td><td>10 ULLMAN</td><td>81</td><td>CNTR Planck-mass 10<sup>19</sup>GeV</td></tr><tr><td></td><td></td><td>10 ULLMAN</td><td>81</td><td>CNTR m ≤ 10<sup>16</sup> GeV</td></tr></tbody></table>

¹ ADRIANI 15 search for relatively light quark matter with charge Z = 1–8. See their Figs. 2 and 3 for flux upper limits.

² AMBROSIO 00b searched for quark matter (“nuclearites”) in the velocity range (10⁻⁵⁻¹) c. The listed limit is for 2 × 10⁻³ c.

³ ASTONE 93 searched for quark matter (“nuclearites”) in the velocity range (10⁻³⁻¹) c. Their Table 1 gives a compilation of searches for nucleartaries.

⁴ AHLEN 92 searched for quark matter (“nuclearites”). The bound applies to velocity < 2.5 × 10⁻³ c. See their Fig. 3 for other velocity/c and heavier mass range.

⁵ NAKAMURA 91 searched for quark matter in the velocity range (4 × 10⁻⁵⁻¹) c.

⁶ ORITO 91 searched for quark matter. The limit is for the velocity range (10⁻⁴⁻10⁻³) c.

⁷ LIU 88 searched for quark matter (“nuclearites”) in the velocity range (2.5 × 10⁻³⁻¹)c. A less stringent limit of 5.8 × 10⁻¹¹ applies for (1–2.5) × 10⁻³ c.

⁸ BARISH 87 searched for quark matter (“nuclearites”) in the velocity range (2.7 × 10⁻⁴⁻⁵ × 10⁻³)c.

⁹ NAKAMURA 85 at KEK searched for quark-matter. These might be lumps of strange quark matter with roughly equal numbers of u, d, s quarks. These lumps or nucleartaries were assumed to have velocity of (10⁻⁴⁻10⁻³)c.

¹⁰ ULLMAN 81 is sensitive for heavy slow singly charge particle reaching earth with vertical velocity 100–350 km/s.

## Highly Ionizing Particle Flux

<table><thead><tr><th>VALUE<br>(cm<sup>-2</sup>γr<sup>-1</sup>)</th><th>CL%</th><th>EVTS</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;0.4</td><td>95</td><td>0</td><td>KINOSHITA</td><td>81B</td><td>PLAS Z/β 30-100</td></tr></tbody></table>

## SEARCHES FOR BLACK HOLE PRODUCTION

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>not seen</td><td>1 AABOUD<br>2 AAD<br>3 AAD<br>4 AAD<br>5 AAD<br>6 AAD<br>7 CHATRCHYAN13A<br>8 CHATRCHYAN13AD<br>9 AAD<br>10 CHATRCHYAN12W<br>11 AAD</td><td>16P ATLS<br>15AN ATLS<br>14A ATLS<br>14AL ATLS<br>14C ATLS<br>13D ATLS<br>12AK ATLS<br>12W CMS<br>11AG ATLS</td><td>13 TeV pp → eµ, eτ, µτ<br>8 TeV pp → multijets<br>8 TeV pp → γ + jet<br>8 TeV pp → ℓ + jet<br>8 TeV pp → ℓ + (ℓ or jets)<br>7 TeV pp → 2 jets<br>7 TeV pp → 2 jets<br>8 TeV pp → multijets<br>8 TeV pp → multijets<br>7 TeV pp → ℓ + (ℓ or jets)<br>7 TeV pp → multijets<br>7 TeV pp → 2 jets</td></tr></tbody></table>

¹ AABOUD 16P set limits on quantum BH production in n = 6 ADD or n = 1 RS models.

² AAD 15AN search for black hole or string ball formation followed by its decay to multijet final states, in pp collisions at $E_{cm} = 8$ TeV with $L = 20.3$ fb⁻¹. See their Figs. 6–8 for limits.

³ AAD 14A search for quantum black hole formation followed by its decay to a γ and a jet, in pp collisions at $E_{cm} = 8$ TeV with $L = 20$ fb⁻¹. See their Fig. 3 for limits.

⁴ AAD 14AL search for quantum black hole formation followed by its decay to a lepton and a jet, in pp collisions at $E_{cm} = 8$ TeV with $L = 20.3$ fb⁻¹. See their Fig. 2 for limits.

⁵ AAD 14C search for microscopic (semiclassical) black hole formation followed by its decay to final states with a lepton and ≥ 2 (leptons or jets), in pp collisions at $E_{cm} = 8$ TeV with $L = 20.3$ fb⁻¹. See their Figures 8–11, Tables 7, 8 for limits.

⁶ AAD 13D search for quantum black hole formation followed by its decay to two jets, in pp collisions at $E_{cm} = 7$ TeV with $L = 4.8$ fb⁻¹. See their Fig. 8 and Table 3 for limits.

⁷ CHATRCHYAN 13A search for quantum black hole formation followed by its decay to two jets, in pp collisions at $E_{cm} = 7$ TeV with $L = 5$ fb⁻¹. See their Figs. 5 and 6 for limits.

⁸ CHATRCHYAN 13AD search for microscopic (semiclassical) black hole formation followed by its evaporation to multiparticle final states, in multijet (including γ, ℓ) events in pp collisions at $E_{cm} = 8$ TeV with $L = 12$ fb⁻¹. See their Figs. 5–7 for limits.

⁹ AAD 12AK search for microscopic (semiclassical) black hole formation followed by its decay to final states with a lepton and ≥ 2 (leptons or jets), in pp collisions at $E_{cm} = 7$ TeV with $L = 1.04$ fb⁻¹. See their Fig. 4 and 5 for limits.

¹⁰ CHATRCHYAN 12W search for microscopic (semiclassical) black hole formation followed by its evaporation to multiparticle final states, in multijet (including γ, ℓ) events in pp collisions at $E_{cm} = 7$ TeV with $L = 4.7$ fb⁻¹. See their Figs. 5–8 for limits.

¹¹ AAD 11AG search for quantum black hole formation followed by its decay to two jets, in pp collisions at $E_{cm} = 7$ TeV with $L = 36$ pb⁻¹. See their Fig. 11 and Table 4 for limits.
REFERENCES FOR Other Particle Searches

<table><thead><tr><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td>AAD</td><td>24B</td><td>PL B848 138324</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23AM</td><td>PR D108 012012</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23AR</td><td>PR D108 032016</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23BQ</td><td>PL B846 138172</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23BT</td><td>PL B847 138316</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23CC</td><td>JHEP 2311 112</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23G</td><td>JHEP 2306 158</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23I</td><td>JHEP 2306 153</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23P</td><td>JHEP 2307 176</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>HAYRAPHET...</td><td>23P</td><td>JHEP 2308 179</td><td>I. Adachi et al. (BELLE II Collab.)</td></tr><tr><td>TUMASYAN</td><td>23A0</td><td>JHEP 2307 210</td><td>A. Hayrapetyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23BC</td><td>JHEP 2312 189</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23BF</td><td>EPJ C83 827</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23G</td><td>JHEP 2305 228</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23I</td><td>JHEP 2307 161</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>AAD</td><td>22G</td><td>PR D105 092012</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>22H</td><td>PR D106 032005</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>22K</td><td>JHEP 2206 005</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>22U</td><td>EPJ C82 606</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>22V</td><td>JHEP 2207 081</td><td>R. Aij et al. (LHCb Collab.)</td></tr><tr><td>ABRATENKO</td><td>22A</td><td>PR D106 092006</td><td>P. Abratenko et al. (MicroBooNE Collab.)</td></tr><tr><td>ACHARYA</td><td>22A</td><td>EPJ C82 694</td><td>B. Acharya et al. (MoEDAL Collab.)</td></tr><tr><td>ALEMANNO</td><td>22</td><td>PR D106 063026</td><td>F. Alemanno et al. (DAMPE Collab.)</td></tr><tr><td>ANDREEV</td><td>22A</td><td>PR L19 161001</td><td>Yu.M. Andreev et al. (NA64 Collab.)</td></tr><tr><td>CAO</td><td>22</td><td>PR L19 261103</td><td>Z. Cao et al. (LHAASO Collab.)</td></tr><tr><td>TUMASYAN</td><td>22AD</td><td>JHEP 2307 081</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22AF</td><td>EPJ C82 153</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22AG</td><td>EPJ C82 213</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22H</td><td>PR D105 112007</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22M</td><td>JHEP 2203 160</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22N</td><td>JHEP 2204 062</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>AAD</td><td>21AL</td><td>PL JHEP 127 051802</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21BA</td><td>JHEP 2111 229</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21F</td><td>PR D103 112006</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21X</td><td>JHEP 2107 173</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21V</td><td>PL JHEP 261 173</td><td>R. Aij et al. (LHCb Collab.)</td></tr><tr><td>ACHARYA</td><td>21</td><td>PL JHEP 126 071801</td><td>B. Acharya et al. (MoEDAL Collab.)</td></tr><tr><td>AFEK</td><td>21</td><td>PR D104 012004</td><td>G. Afek et al. (YALE)</td></tr><tr><td>ALKHATIB</td><td>21</td><td>PR L127 081802</td><td>I. Alkhatib et al. (SuperCDMS Collab.)</td></tr><tr><td>ANDREEV</td><td>21</td><td>PR L126 211802</td><td>Yu.M. Andreev et al. (NA64 Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21AF</td><td>PR D104 052101</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21A</td><td>PR D104 0629</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21U</td><td>PR D104 012015</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>21U</td><td>PR D104 216804</td><td>A. Tumasyan et al. (CMS Collab.)</td></tr><tr><td>AAD</td><td>20AD</td><td>PL R125 131801</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20D</td><td>PL B801 135114</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20U</td><td>PR D99 052013</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20P</td><td>PR D102 032006</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20M</td><td>EPJ C80 450</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20T</td><td>JHEP 2003 145</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20W</td><td>JHEP 2006 151</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20Z</td><td>JHEP 2007 156</td><td>R. Aij et al. (LHCb Collab.)</td></tr><tr><td>AGUILAR-AR...</td><td>20B</td><td>JHEP 2004 054</td><td>A. Aguilar-Arevalo et al. (CONNIE Collab.)</td></tr><tr><td>BALL</td><td>20</td><td>JHEP 2002 03200</td><td>A.H. Ball et al. (millQan)</td></tr><tr><td>FEDDERKE</td><td>20</td><td>PR D101 115021</td><td>M.A. Fedderke, P.W. Graham, S. Rajendran (STAN+)</td></tr><tr><td>SIRUNYAN</td><td>20A</td><td>EPJ C80 3</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20AI</td><td>JHEP 2005 033</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20BT</td><td>PL B847 135578</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20C</td><td>EPJ C80 75</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20N</td><td>PL B806 135502</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20Z</td><td>JHEP 2003 051</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>AABOUD</td><td>19AA</td><td>EPJ C79 120</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19AE</td><td>EPJ C79 451</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19AJ</td><td>PL B795 56</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19AK</td><td>PL R122 158101</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19AM</td><td>PR D99 052003</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19AO</td><td>PR D99 052005</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19AT</td><td>PR D99 092007</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19G</td><td>PR D99 012001</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19H</td><td>PR D99 012008</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19Q</td><td>JHEP 1905 041</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19V</td><td>JHEP 1905 142</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>ALCANTARA</td><td>19</td><td>JHEP 1903 0106</td><td>E. Alcantara, L.A. Anchordoqui, J.F. Soriano</td></tr><tr><td>SIRUNYAN</td><td>19B</td><td>PR D108 012005</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19BH</td><td>PR D99 032011</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19BT</td><td>PL B797 134876</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19CA</td><td>PR D100 112003</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19CD</td><td>PL R123 231903</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19E</td><td>PR D99 092001</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19Q</td><td>JHEP 1902 179</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>AABOUD</td><td>18AD</td><td>PL B779 24</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18CJ</td><td>PR D98 052008</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18CK</td><td>PR D98 092002</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18CL</td><td>PR D98 092005</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18N</td><td>PR D98 092008</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18N</td><td>PL D121 081801</td><td>R. Aij et al. (LHCb Collab.)</td></tr><tr><td>AAJ</td><td>18AJ</td><td>PR L120 068101</td><td>A. Albert et al. (HAWC Collab.)</td></tr><tr><td>ALBERT</td><td>18C</td><td>PR D98 123012</td><td>M. Aaboud et al. (HAWC Collab.)</td></tr><tr><td>ALVIS</td><td>18</td><td>PR L120 211804</td><td>S.I. Avis et al. (MAJORANA Collab.)</td></tr><tr><td>BANERJEE</td><td>18A</td><td>PR L120 231802</td><td>D. Banerjee et al. (NA64 Collab.)</td></tr><tr><td>BANERJEE</td><td>18B</td><td>JHEP 097 02022</td><td>D. Banerjee et al. (NA64 Collab.)</td></tr><tr><td>KILE</td><td>18</td><td>JHEP 1810 116</td><td>J. Kile, J. von Wimmersperg-Toeller (LISBT)</td></tr><tr><td>MARSICANO</td><td>18</td><td>JHEP 1805 0153</td><td>L. Marsicano et al. (PPTA Collab.)</td></tr><tr><td>PORAYKO</td><td>18A</td><td>PR D98 102002</td><td>N.K. Porayako et al. (PPTA Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18W</td><td>PL C31 127</td><td>ZPHY C31 21</td></tr><tr><td>SIRUNYAN</td><td>18BB</td><td>PR D96 180 120</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18DA</td><td>JHEP 1811 042</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18DD</td><td>EPJ C78 789</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18DJ</td><td>JHEP 1809 101</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18DR</td><td>JHEP 1811 161</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18DU</td><td>JHEP 092001</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18DY</td><td>PR D98 112014</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18ED</td><td>JHEP 1811 172</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>AABOUD</td><td>17D</td><td>PL B765 32</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>17B</td><td>PR D95 032001</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>17T</td><td>JHEP 1708 052</td><td>M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AAJ</td><td>17BR</td><td>EPJ C77 812</td><td>R. Aij et al. (LHCb Collab.)</td></tr><tr><td>AAJIKIM</td><td>17AA</td><td>PL B774 252</td><td>A. Ablikim et al. (BESIII Collab.)</td></tr><tr><td>KHACHATRY...</td><td>17D</td><td>JHEP 1701 076</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>KHACHATRY...</td><td>17W</td><td>JHEP 2769 520</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>KHACHATRY...</td><td>17H</td><td>JHEP 2769 520</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>17B</td><td>JHEP 1704 136</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>17C</td><td>JHEP 1705 029</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>17F</td><td>JHEP 1707 013</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>17J</td><td>JHEP 1707 073</td><td>A.M. Sirunyan et al. (CMS Collab.)</td></tr><tr><td>ZANG</td><td>17</td><td>PL B773 159</td><td>X. Zang, G.A. Miller (WASH)</td></tr><tr><td>AABOUD</td><td>16</td><td>EP J76 229</td><td>A.M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>16P</td><td>EP J76 541</td><td>A.M. Aaboud et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16AI</td><td>JHEP 1603 041</td><td>G. Aad et al. (ATLAS Collab.)</td></tr></tbody></table>

<table><tbody><tr><td>AAD</td><td>16N</td><td>JHEP 1603 026</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16O</td><td>PL B760 520</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16R</td><td>PL B755 285</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16S</td><td>PL B754 302</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAIJ</td><td>16AR</td><td>EPJ C76 664</td><td>R. Aaij et al. (LHCb Collab.)</td></tr><tr><td>KHACHATRY...</td><td>16BW</td><td>PR D94 112004</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>KHACHATRY...</td><td>16K</td><td>PL R116 071801</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>KHACHATRY...</td><td>16L</td><td>PL R117 031802</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>KHACHATRY...</td><td>16M</td><td>PL R117 051802</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>KRASZNAHO...</td><td>16</td><td>PL R116 042501</td><td>A.J. Krasznahorayk et al. (HINR, ANIK+)</td></tr><tr><td>AAD</td><td>15AN</td><td>JHEP 1507 032</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15AT</td><td>EPJ C75 79</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15BJ</td><td>EPJ C75 362</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAIJ</td><td>15B</td><td>EPJ C75 595</td><td>R. Aaij et al. (LHCb Collab.)</td></tr><tr><td>ADRIANI</td><td>15</td><td>PL R115 111101</td><td>O. Adriani et al. (PAMELA Collab.)</td></tr><tr><td>AGNESE</td><td>15</td><td>PL R114 111302</td><td>R. Agnese et al. (CDMS Collab.)</td></tr><tr><td>KHACHATRY...</td><td>15L</td><td>PL R14 101801</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>LEES</td><td>15E</td><td>PL R114 171801</td><td>J.P. Lees et al. (BABAR Collab.)</td></tr><tr><td>AAD</td><td>14A</td><td>PL B728 562</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>14L</td><td>PL R112 091804</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>14C</td><td>JHEP 1408 103</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AALTONEN</td><td>14J</td><td>PR D89 092001</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AAD</td><td>14L</td><td>PL B78 860</td><td>A.A. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AAD</td><td>13AH</td><td>PL B722 305</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>13C</td><td>PL R110 011802</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>13D</td><td>JHEP 1301 029</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AALTONEN</td><td>13I</td><td>PR D88 031103</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>13L</td><td>PL R111 031802</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>13</td><td>PL B718 815</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>13A</td><td>PL JHEP 1301 013</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>13AB</td><td>JHEP 1307 122</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>Also</td><td>13AD</td><td>JHEP 2211 149 (errat.)</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>13AF</td><td>JHEP 1307 178</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>13AR</td><td>PR D87 092008</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>Also</td><td>13AF</td><td>PR D106 099903 (errat.)</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>AAD</td><td>12AK</td><td>PL B716 122</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>12C</td><td>PL R108 041102</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>12S</td><td>PL B708 37</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AALTONEN</td><td>12C</td><td>PL DCF 111804</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>12AP</td><td>JHEP 1209 094</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>12BL</td><td>JHEP 1212 015</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>12Q</td><td>PL B716 260</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>12T</td><td>PL R108 261803</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>12U</td><td>JHEP 204 061</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>AAD</td><td>11AG</td><td>NJP 13 053044</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>11I</td><td>PL B698 353</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AAD</td><td>11S</td><td>PL B705 294</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AALTONEN</td><td>11AF</td><td>PL R107 181801</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>11M</td><td>PL R106 171801</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>ABAZOV</td><td>11P</td><td>PL R107 011804</td><td>V.M. Abazov et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>11C</td><td>JHEP 1106 026</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>CHATRYCHY...</td><td>11U</td><td>PL R107 201804</td><td>S. Chatrychyan et al. (CMS Collab.)</td></tr><tr><td>AAD</td><td>10</td><td>PL R105 161801</td><td>G. Aad et al. (ATLAS Collab.)</td></tr><tr><td>AALTONEN</td><td>10AF</td><td>PR D82 052005</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>KHACHATRY...</td><td>10</td><td>PL R105 211801</td><td>V. Khachatryan et al. (CMS Collab.)</td></tr><tr><td>Also</td><td>10AF</td><td>PL R80 011102</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>09G</td><td>PR D79 052004</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>09Z</td><td>PL R103 021802</td><td>T. Aaltonen et al. (CDF Collab.)</td></tr><tr><td>ABAZOV</td><td>09M</td><td>PL R102 161802</td><td>V.M. Abazov et al. (H1 Collab.)</td></tr><tr><td>AKTAS</td><td>04C</td><td>EPJ C36 413</td><td>A. Atkas et al. (CMS Collab.)</td></tr><tr><td>JAVORSEK</td><td>02</td><td>PR D65 072003</td><td>D. Javorsek II et al. (CMS Collab.)</td></tr><tr><td>JAVORSEK</td><td>01</td><td>PR D64 012005</td><td>D. Javorsek II et al. (CMS Collab.)</td></tr><tr><td>JAVORSEK</td><td>01B</td><td>PL 87 231804</td><td>D. Javorsek II et al. (CMS Collab.)</td></tr><tr><td>ABBIENDO</td><td>00B</td><td>EPJ C13 197</td><td>G. Abbiendi et al. (MACRO Collab.)</td></tr><tr><td>ANDROSIO</td><td>00B</td><td>EPJ C13 453</td><td>F. Ambroso et al. (CMS Collab.)</td></tr><tr><td>ABE</td><td>99F</td><td>PL 82 2038</td><td>F. Abe et al. (OPAL Collab.)</td></tr><tr><td>ACKERSTAFF</td><td>98P</td><td>PL B433 195</td><td>K. Ackerstaff et al. (OPAL Collab.)</td></tr><tr><td>ABE</td><td>97G</td><td>PL D55 5263</td><td>F. Abe et al. (OPAL Collab.)</td></tr><tr><td>ABREU</td><td>97D</td><td>PL B396 315</td><td>P. Abreu et al. (DELPHI Collab.)</td></tr><tr><td>ACKERSTAFF</td><td>97D</td><td>PL B39 210</td><td>K. Ackerstaff et al. (OPAL Collab.)</td></tr><tr><td>ADAMS</td><td>97B</td><td>PL 79 4083</td><td>F.NAL KTeV et al. (HELIOS Collab.)</td></tr><tr><td>BARATE</td><td>97K</td><td>PL B405 379</td><td>R. Barate et al. (ALEPH Collab.)</td></tr><tr><td>AKESSON</td><td>95K</td><td>ZPHY C67 203</td><td>R. Akers et al. (OPAL Collab.)</td></tr><tr><td>GALLAS</td><td>95</td><td>PR D52 6</td><td>E. Gallas et al. (MSU, FNAL, MIT, FLOR) (EPA, TRIU)</td></tr><tr><td>RAM</td><td>94</td><td>PL D12 3120</td><td>S. Ram et al. (CMS Collab.)</td></tr><tr><td>ABE</td><td>93G</td><td>PL 71 2542</td><td>F. Abe et al. (CDF Collab.)</td></tr><tr><td>ASTONE</td><td>93</td><td>PL D47 4770</td><td>P. Astone et al. (ROMA, ROMAI, CATA, FRAS)</td></tr><tr><td>BUSKULIC</td><td>93C</td><td>PL B30 198</td><td>D. Buskulic et al. (ALEPH Collab.)</td></tr><tr><td>YAMAGATA</td><td>93</td><td>PR D47 1231</td><td>T. Yamagata, Y. Takamori, H. Utsunomiya (KONAN)</td></tr><tr><td>ABE</td><td>92</td><td>PR D46 1889</td><td>F. Abe et al. (CMS Collab.)</td></tr><tr><td>ADEN</td><td>93</td><td>PL D5 1860</td><td>S.P. Akh et al. (MACRO Collab.)</td></tr><tr><td>VERKERK</td><td>92</td><td>PL R68 1116</td><td>P. Verkerk et al. (ENSP, SALC, PAST)</td></tr><tr><td>AKESSON</td><td>91</td><td>ZPHY C52 219</td><td>T. Akesson et al. (ROCH, MICCH, OHIO+)</td></tr><tr><td>NAKAMURA</td><td>91</td><td>PL B263 529</td><td>T. Saito et al. (ICRR, KOBE)</td></tr><tr><td>ORITO</td><td>91</td><td>PR D6 1951</td><td>T.T. Nakamura et al. (KYOT, TMTC)</td></tr><tr><td>ADACHI</td><td>90E</td><td>PL B244 352</td><td>E.B. Norman et al. (LBL)</td></tr><tr><td>ADACHI</td><td>90E</td><td>PL B249 336</td><td>BERNSTEIN et al. (STAN, WISC)</td></tr><tr><td>AKRAWY</td><td>90E</td><td>PL B252 290</td><td>R.M. Stein et al. (STAN, WISC)</td></tr><tr><td>HEMMICK</td><td>90</td><td>PL D41 2074</td><td>G. Liu, B. Barish (CIT)</td></tr><tr><td>SAITO</td><td>90</td><td>PR D5 2094</td><td>B.C. Barish, G. Liu, C. Lane (CIT)</td></tr><tr><td>NAKAMURA</td><td>91</td><td>PL D36 2641</td><td>E.B. Norman, S.B. Gazes, D.A. Bennett (LBL)</td></tr><tr><td>ORITO</td><td>91</td><td>PL D6 1951</td><td>J. Badler et al. (NA3 Collab.)</td></tr><tr><td>ADACHI</td><td>91B</td><td>PL B23 21</td><td>A. Mincer et al. (UMD, GMAS, NSF)</td></tr><tr><td>NAKAMURA</td><td>85</td><td>PL D32 541</td><td>K. Nakamura et al. (KEK, INUS)</td></tr><tr><td>THRON</td><td>85</td><td>PL D161 417</td><td>J.L. Thron et al. (YALE, FNAL, IOWA)</td></tr><tr><td>SAKUYAMA</td><td>85B</td><td>PL D31 451</td><td>H. Sakuyama, N. Suzuki (MEIS)</td></tr><tr><td>Also</td><td>85</td><td>LNC 37 17</td><td>H. Sakuyama, K. Watanabe (MEIS)</td></tr><tr><td>Also</td><td>85</td><td>LNC 36 389</td><td>H. Sakuyama, K. Watanabe (MEIS)</td></tr><tr><td>Also</td><td>85</td><td>NC 78A 147</td><td>H. Sakuyama, K. Watanabe (MEIS)</td></tr><tr><td>BHAT</td><td>82</td><td>PL D25 2820</td><td>P.N. Bhat et al. (TATA)</td></tr><tr><td>KINOSHITA</td><td>82</td><td>PL R48 77</td><td>K. Kinoshita, P.B. Price, D. Fryberger (UCB+)</td></tr><tr><td>MARINI</td><td>82</td><td>PR D26 1777</td><td>A. Marini et al. (FRAS, LBL, NWES, STAN+)</td></tr><tr><td>SIMIT</td><td>82B</td><td>NP D206 333</td><td>P.F. Sehgal et al. (RAL)</td></tr><tr><td>KINOSHITA</td><td>81B</td><td>PL D24 1707</td><td>K. Kinoshita, P.B. Price (UCB)</td></tr><tr><td>LOSECCO</td><td>81</td><td>PL D12 209</td><td>J.M. LoSecco et al. (MICH, PENN, BNL)</td></tr><tr><td>ULLMAN</td><td>81</td><td>PL R47 289</td><td>J.D. Ullman (LEHM, BNL)</td></tr><tr><td>YOCK</td><td>81</td><td>PL R23 1207</td><td>P.C.M. Yock (AUCK)</td></tr><tr><td>BARJOL</td><td>81</td><td>ZPHY C6 295</td><td>W. Bartel et al. (JADE Collab.)</td></tr><tr><td>BUSSIERE</td><td>80</td><td>NP B174 1</td><td>A. Bussiere et al. (BGNA, SACL, LAPP)</td></tr><tr><td>YOCK</td><td>80</td><td>PL D22 61</td><td>P.C.M. Yock (AUCK)</td></tr><tr><td>ARMITAGE</td><td>79</td><td>NP B150 87</td><td>J.C.M. Armitage et al. (CERN, DARE, FOM+)</td></tr><tr><td>BOZZOLI</td><td>79</td><td>NP B159 363</td><td>W. Bozzoli et al. (BGNA, LAPP, SACL+)</td></tr><tr><td>GOODMAN</td><td>79</td><td>PR D19 572</td><td>J.A. Goodman et al. (UMD)</td></tr><tr><td>SMITH</td><td>79</td><td>NP B149 525</td><td>P.F. Smith, J.R.J. Bennett (RHEL)</td></tr><tr><td>BHAT</td><td>78</td><td>PRAM 10 115</td><td>P.N. Bhat, P.V. Ramana Murthy (TATA)</td></tr><tr><td>CARROLL</td><td>78</td><td>PL R41 777</td><td>A.S. Carroll et al. (BNL, PRIN)</td></tr></tbody></table>
# Searches Particle Listings

## Other Particle Searches

CUTTS 78 PRL 41 363

VIDAL 78 PL 77B 344

ALEKSEEV 76 SJNP 22 531

ALEKSEEV 76B SJNP 23 633

BALDIN 76 SJNP 22 264

BRIATORE 76 NC 31A 553

GUSTAFSON 76 PRL 37 474

ALBROW 75 NP B97 189

FRANKEL 75 PR D12 2561

JOVANOV... 75 PL 56B 105

YOCK 75 NP B86 216

D. Cutts et al.

R.A. Vidal et al.

G.D. Alekseev et al.

G.D. Alekseev et al.

G.D. Alekseev et al.

B.Y. Baldin et al.

L. Briatore et al.

H.R. Gustafson et al.

M.G. Albrow et al.

S. Frankel et al.

J.V. Jovanovich et al.

(BROW, FNAL, ILL, BARI+)

(COLU, FNAL, STON+)

(JINR)

(JINR)

(JINR)

(JINR)

(LCGT, FRAS, FREIB)

(MICH)

(CERN, DARE, FOM+)

(PENN, FNAL)

(MANI, AACH, CERN+)

(AUCK, SLAC)

APPEL 74 PRL 32 428

FRANKEL 74 PR D9 1932

YOCK 74 NP B76 175

ALPER 73 PL 46B 265

LEIPUNER 73 PRL 31 1226

DARDO 72 NC 9A 319

TONWAR 72 JP A5 569

ANTIPOV 71B NP B31 235

ANTIPOV 71C PL 34B 164

BINON 69 PL 30B 510

BJORNBOE 68 NC B53 241

JONES 67 PR 164 1584

DORFAN 65 PRL 14 999

J.A. Appel et al. (COLU, FNAL)

S. Frankel et al. (PENN, FNAL)

P.C.M. Yock (AUCK)

B. Alper et al. (CERN, LIVP, LUND, BOHR+)

L.B. Lelpuner et al. (BNL, YALE)

M. Dardo et al. (TORI)

S.C. Tonwar, S. Naranan, B.V. Sreekantan (TATA)

Y.M. Antipov et al. (SERP)

Y.M. Antipov et al. (SERP)

F.G. Binon et al. (SERP)

J. Bjornboe et al. (BOHR, TATA, BERN+)

L.W. Jones (MICH, WISC, LBL, UCLA, MINN+)

(COLU)