# Searches Particle Listings

## Supersymmetric Particle Searches

<table><tbody><tr><td>&gt;2500</td><td>95</td><td>7 SIRUNYAN</td><td>19BT CMS</td><td>long-lived <span style="text-decoration: overline;">g</span>, GMSB, <span style="text-decoration: overline;">g</span> → gG, cτ = 1 m</td></tr><tr><td>&gt;1900</td><td>95</td><td>7 SIRUNYAN</td><td>19BT CMS</td><td>long-lived <span style="text-decoration: overline;">g</span>, GMSB, <span style="text-decoration: overline;">g</span> → gG, cτ = 100 m</td></tr><tr><td>&gt;2370</td><td>95</td><td>8 AABOUD</td><td>18S ATLS</td><td>displaced vertex + <span style="text-decoration: overline;">E</span><sub>T</sub>, long-lived Tglu1A, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV, and τ=0.17 ns</td></tr><tr><td>&gt;1600</td><td>95</td><td>9 SIRUNYAN</td><td>18AY CMS</td><td>jets+<span style="text-decoration: overline;">E</span><sub>T</sub>, Tglu1A, cτ &lt; 0.1 mm, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1750</td><td>95</td><td>9 SIRUNYAN</td><td>18AY CMS</td><td>jets+<span style="text-decoration: overline;">E</span><sub>T</sub>, Tglu1A, cτ = 1 mm, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1640</td><td>95</td><td>9 SIRUNYAN</td><td>18AY CMS</td><td>jets+<span style="text-decoration: overline;">E</span><sub>T</sub>, Tglu1A, cτ = 10 mm, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1490</td><td>95</td><td>9 SIRUNYAN</td><td>18AY CMS</td><td>jets+<span style="text-decoration: overline;">E</span><sub>T</sub>, Tglu1A, cτ = 100 mm, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1300</td><td>95</td><td>9 SIRUNYAN</td><td>18AY CMS</td><td>jets+<span style="text-decoration: overline;">E</span><sub>T</sub>, Tglu1A, cτ = 1 m, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;960</td><td>95</td><td>9 SIRUNYAN</td><td>18AY CMS</td><td>jets+<span style="text-decoration: overline;">E</span><sub>T</sub>, Tglu1A, cτ = 10 m, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;900</td><td>95</td><td>9 SIRUNYAN</td><td>18AY CMS</td><td>jets+<span style="text-decoration: overline;">E</span><sub>T</sub>, Tglu1A, cτ = 100 m, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;2200</td><td>95</td><td>10 SIRUNYAN</td><td>18DV CMS</td><td>long-lived <span style="text-decoration: overline;">g</span>, RPV, <span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">d</span><span style="text-decoration: overline;">s</span>, 0.6 mm &lt; cτ &lt; 80 mm</td></tr><tr><td>&gt;1000</td><td>95</td><td>11 KHACHATRY...17AR CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span>, RPV, <span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">d</span><span style="text-decoration: overline;">s</span>, cτ = 0.3 mm</td></tr><tr><td>&gt;1300</td><td>95</td><td>11 KHACHATRY...17AR CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span>, RPV, <span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">d</span><span style="text-decoration: overline;">s</span>, cτ = 1.0 mm</td></tr><tr><td>&gt;1400</td><td>95</td><td>11 KHACHATRY...17AR CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span>, RPV, <span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">d</span><span style="text-decoration: overline;">s</span>, 2 mm &lt; cτ &lt; 30 mm</td></tr><tr><td>&gt;1580</td><td>95</td><td>12 AABOUD</td><td>16B ATLS</td><td>long-lived R-hadrons</td></tr><tr><td>&gt;740-1590</td><td>95</td><td>13 AABOUD</td><td>16C ATLS</td><td>R-hadrons, Tglu1A, τ ≥ 0.4 ns, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1570</td><td>95</td><td>13 AABOUD</td><td>16C ATLS</td><td>R-hadrons, Tglu1A, stable</td></tr><tr><td>&gt;1610</td><td>95</td><td>14 KHACHATRY...16BW CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span> forming R-hadrons, f = 0.1, cloud interaction model</td></tr><tr><td>&gt;1580</td><td>95</td><td>14 KHACHATRY...16BW CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span> forming R-hadrons, f = 0.1, charge-suppressed interaction model</td></tr><tr><td>&gt;1520</td><td>95</td><td>14 KHACHATRY...16BW CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span> forming R-hadrons, f = 0.5, cloud interaction model</td></tr><tr><td>&gt;1540</td><td>95</td><td>14 KHACHATRY...16BW CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span> forming R-hadrons, f = 0.5, charge-suppressed interaction model</td></tr><tr><td>&gt;1270</td><td>95</td><td>15 AAD</td><td>15AE ATLS</td><td><span style="text-decoration: overline;">g</span> R-hadron, generic R-hadron model</td></tr><tr><td>&gt;1360</td><td>95</td><td>15 AAD</td><td>15AE ATLS</td><td><span style="text-decoration: overline;">g</span> decaying to 300 GeV stable sleptons, LeptoSUSY model</td></tr><tr><td>&gt;1115</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> R-hadron, stable</td></tr><tr><td>&gt;1185</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → (g/q<span style="text-decoration: overline;">q</span>)χ̃<sub>1</sub><sup>0</sup>, lifetime 10 ns, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1099</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → (g/q<span style="text-decoration: overline;">q</span>)χ̃<sub>1</sub><sup>0</sup>, lifetime 10 ns, m<sub>χ̃</sub><sup>0</sup> = m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1182</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">t</span>χ̃<sub>1</sub><sup>0</sup>, lifetime 10 ns, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1157</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">t</span>χ̃<sub>1</sub><sup>0</sup>, lifetime 10 ns, m<sub>χ̃</sub><sup>0</sup> = m<sub>χ̃1</sub><sup>0</sup> = 480 GeV</td></tr><tr><td>&gt;869</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → (g/q<span style="text-decoration: overline;">q</span>)χ̃<sub>1</sub><sup>0</sup>, lifetime 1 ns, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;821</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → (g/q<span style="text-decoration: overline;">q</span>)χ̃<sub>1</sub><sup>0</sup>, lifetime 1 ns, m<sub>χ̃</sub><sup>0</sup> = m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;836</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">t</span>χ̃<sub>1</sub><sup>0</sup>, lifetime 1 ns, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;836</td><td>95</td><td>16 AAD</td><td>15BM ATLS</td><td><span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">t</span>χ̃<sub>1</sub><sup>0</sup>, lifetime 10 ns, m<sub>χ̃</sub><sup>0</sup> = m<sub>χ̃1</sub><sup>0</sup> = 480 GeV</td></tr><tr><td>&gt;1000</td><td>95</td><td>17 KHACHATRY...15AK CMS</td><td></td><td><span style="text-decoration: overline;">g</span> R-hadrons, 10 µs &lt; τ &lt; 1000 s</td></tr><tr><td>&gt;880</td><td>95</td><td>17 KHACHATRY...15AK CMS</td><td></td><td><span style="text-decoration: overline;">g</span> R-hadrons, 1 µs &lt; τ &lt; 1000 s limits, etc. • • •</td></tr><tr><td>&gt;985</td><td>95</td><td>18 AAD</td><td>13AA ATLS</td><td><span style="text-decoration: overline;">g</span>, R-hadrons, generic interaction model</td></tr><tr><td>&gt;832</td><td>95</td><td>19 AAD</td><td>13BC ATLS</td><td>R-hadrons, <span style="text-decoration: overline;">g</span> → g/q<span style="text-decoration: overline;">q</span>χ̃<sub>1</sub><sup>0</sup>, generic R-hadron model, lifetime between 10<sup>-5</sup> and 10<sup>3</sup> s, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;1322</td><td>95</td><td>20 CHATRCHYAN 13AB CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span> forming R-hadrons, f = 0.1, cloud interaction model</td></tr><tr><td>none 200-341</td><td>95</td><td>21 AAD</td><td>12P ATLS</td><td>long-lived <span style="text-decoration: overline;">g</span> → gχ̃<sub>1</sub><sup>0</sup>, m<sub>χ̃1</sub><sup>0</sup> = 100 GeV</td></tr><tr><td>&gt;640</td><td>95</td><td>22 CHATRCHYAN 12AN CMS</td><td></td><td>long-lived <span style="text-decoration: overline;">g</span> → gχ̃<sub>1</sub><sup>0</sup></td></tr></tbody></table>

<table><tbody><tr><td>&gt;1098</td><td>95</td><td>23 CHATRCHYAN 12L CMS</td><td>long-lived <span style="text-decoration: overline;">g</span> forming R-hadrons, f = 0.1</td></tr><tr><td>&gt;586</td><td>95</td><td>24 AAD</td><td>11k ATLS</td><td>stable <span style="text-decoration: overline;">g</span></td></tr><tr><td>&gt;544</td><td>95</td><td>25 AAD</td><td>11P ATLS</td><td>stable <span style="text-decoration: overline;">g</span>, GMSB scenario, tanβ=5</td></tr><tr><td>&gt;370</td><td>95</td><td>26 KHACHATRY...11 CMS</td><td>long lived <span style="text-decoration: overline;">g</span></td></tr><tr><td>&gt;398</td><td>95</td><td>27 KHACHATRY...11c CMS</td><td>stable <span style="text-decoration: overline;">g</span></td></tr></tbody></table>

1. AAD 23G searched in 139 fb⁻¹ of pp collisions at √s = 13 TeV for R-hadron pair production in events with high-pt tracks with large ionisation in the pixel detector. No significant excess above the Standard Model predictions is observed. Limits are set on the R-hadron mass for different masses of the LSP and for different R-hadron lifetimes, see Figure 18.

2. SIRUNYAN 21AF searched in 140 fb⁻¹ of pp collisions at √s = 13 TeV for supersymmetry in events with two displaced vertices from long-lived particles decaying into multijet or dijet final states. No significant excess above the Standard Model expectations is observed. Limits are set on long-lived gluinos in an RPC GMSB SUSY model of gluino pair production, with <span style="text-decoration: overline;">g</span> → gG, see their Figure 9, in Tglu1A in a mini-split model, see their Figure 10, and in an RPV model of gluino pair production, with <span style="text-decoration: overline;">g</span> → tbs with coupling λ''<sub>323</sub>, see their Figure 11. Limits are also set on long-lived top squarks in Tstop2RPV, see their Figure 12, in an RPV model with <span style="text-decoration: overline;">t</span> → d<span style="text-decoration: overline;">t</span> and λ''<sub>313</sub> coupling, see their Figure 13, and a dynamical RPV model with <span style="text-decoration: overline;">t</span> → d<span style="text-decoration: overline;">d</span> via a nonholomorphic RPV coupling η''<sub>311</sub>, see their Figure 14. The best mass limit is achieved in all cases at cτ = 30 mm.

3. SIRUNYAN 21U searched in 132 fb⁻¹ of pp collisions at √s = 13 TeV for supersymmetry in events with displaced tracks and displaced vertices associated with a dijet system. No significant excess above the Standard Model expectations is observed. Limits are set on long-lived gluinos in an RPC GMSB SUSY model of gluino pair production, with <span style="text-decoration: overline;">g</span> → gG, see their Figure 9, in Tglu1A in a mini-split model, see their Figure 10, and in an RPV model of gluino pair production, with <span style="text-decoration: overline;">g</span> → tbs with coupling λ''<sub>323</sub>, see their Figure 11. Limits are also set on long-lived top squarks in Tstop2RPV, see their Figure 12, in an RPV model with <span style="text-decoration: overline;">t</span> → d<span style="text-decoration: overline;">t</span> and λ''<sub>313</sub> coupling, see their Figure 13, and a dynamical RPV model with <span style="text-decoration: overline;">t</span> → d<span style="text-decoration: overline;">d</span> via a nonholomorphic RPV coupling η''<sub>311</sub>, see their Figure 14. The best mass limit is achieved in all cases at cτ = 30 mm.

4. AABOUD 19AT searched in 36.1 fb⁻¹ of pp collisions at √s = 13 TeV for metastable and stable R-hadrons. Multiple search strategies for a wide range of lifetimes, corresponding to path lengths of a few meters, are defined. No significant deviations from the expected Standard Model background are observed. Gluino R-hadrons with lifetimes of the order of 50 ns are excluded at 95% C.L. for masses below 1980 GeV using the muon-spectrometer agnostic analysis. Using the full-detector search, the observed lower limits on the mass are 2000 GeV. See their Figure 9 (top).

5. AABOUD 19C searched in 36.1 fb⁻¹ of pp collisions at √s = 13 TeV for metastable and stable R-hadrons arising as excesses in the mass distribution of reconstructed tracks with high transverse momentum and large dE/dx. Gluino R-hadrons with lifetimes above 10 ns are excluded at 95% C.L. with lower mass limit range between 1000 GeV and 2060 GeV, see their Figure 5(a). Masses smaller than 1290 GeV are excluded for a lifetime of 1 ns, see their Figure 6. In the case of stable R-hadrons, the lower mass limit is 1890 GeV, see their Figure 5(b).

6. SIRUNYAN 19BH searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for long-lived particles decaying into jets, with each long-lived particle having a decay vertex well displaced from the production vertex. The selected events are found to be consistent with standard model predictions. Limits are set on the gluino mass in a GMSB model where the gluino is decaying via <span style="text-decoration: overline;">g</span> → g<span style="text-decoration: overline;">G</span>, see their Figure 4 and in an RPV model of supersymmetry where the gluino is decaying via <span style="text-decoration: overline;">g</span> → <span style="text-decoration: overline;">t</span><span style="text-decoration: overline;">d</span><span style="text-decoration: overline;">s</span>, see their Figures 5. Limits are also set on the stop mass in two RPV models, see their Figure 6 (for t → b<span style="text-decoration: overline;">t</span> decays) and Figure 7 (for <span style="text-decoration: overline;">t</span> → d<span style="text-decoration: overline;">d</span> decays).

7. SIRUNYAN 19Bt searched in 137 fb⁻¹ of pp collisions at √s = 13 TeV for long-lived particles decaying to displaced, nonprompt jets and missing transverse momentum. Candidate signal events are identified using the timing capabilities of the CMS electromagnetic calorimeter. The results of the search are found to be consistent with the background predictions. Limits are set on the gluino mass in a GMSB model where long-lived gluinos are pair produced and decaying via <span style="text-decoration: overline;">g</span> → g<span style="text-decoration: overline;">G</span>, see their Figures 4 and 5.

8. AABOUD 18S searched in 32.8 fb⁻¹ of pp collisions at √s = 13 TeV for long-lived gluinos in final states with large missing transverse momentum and at least one high-mass displaced vertex with five or more tracks. The observed yield is consistent with the expected background. Exclusion limits are derived for Tglu1A models predicting the existence of long-lived gluinos reaching roughly m(g̃) = 2000 GeV to 2370 GeV for m(χ̃<sub>1</sub><sup>0</sup>) = 100 GeV and gluino lifetimes between 0.02 and 10 ns, see their Fig. 8. Limits are presented also as a function of the lifetime (for a fixed gluino-neutralino mass difference of 100 GeV) and of the gluino and neutralino masses (for a fixed lifetime of 1 ns). See their Fig. 9 and 10 respectively.

9. SIRUNYAN 18AY searched in 35.9 fb⁻¹ of pp collisions at √s = 13 TeV for events containing one or more jets and significant <span style="text-decoration: overline;">E</span><sub>T</sub>. No significant excess above the Standard Model expectations is observed. Limits are set on the gluino mass in the Tglu1A, Tglu2A and Tglu3A simplified models, see their Figure 3. Limits are also set on squark, sbottom and stop masses in the Tsqk1, Tsbt01, Tstop1 and Tstop4 simplified models, see their Figure 3. Finally, limits are set on long-lived gluino masses in a Tglu1A simplified model where the gluino is metastable or long-lived with proper decay lengths in the range 10⁻³ mm &lt; cτ &lt; 10⁵ mm, see their Figure 4.

10. SIRUNYAN 18DV searched in 38.5 fb⁻¹ of pp collisions at √s = 13 TeV for long-lived particles in events with multiple jets and two displaced vertices composed of many tracks. No events with two well-separated high-track-multiplicity vertices were observed. Limits are set on the stop and the gluino mass in RPV models of supersymmetry where the stop (gluino) is decaying solely into dijet (multijet) final states, see their Figures 6 and 7.

11. KHACHATRY 17AR searched in 17.6 fb⁻¹ of pp collisions at √s = 8 TeV for R-parity-violating SUSY in which long-lived neutralinos or gluinos decay into multijet final states. No significant excess above the Standard Model expectations is observed. Limits are set on the gluino mass for a range of mean proper decay lengths (cτ), see their Fig. 7. The upper limits on the production cross section times branching ratio squared (Fig. 7) are also applicable to long-lived neutralinos.

12. AABOUD 16B searched in 3.2 fb⁻¹ of pp collisions at √s = 13 TeV for long-lived R-hadrons using observables related to large ionization losses and slow propagation velocities, which are signatures of heavy charged particles traveling significantly slower than the speed of light. Exclusion limits at 95% C.L. are set on the long-lived gluino masses exceeding 1580 GeV. See their Fig. 5.

13. AABOUD 16C searched in 3.2 fb⁻¹ of pp collisions at √s = 13 TeV for long-lived and stable R-hadrons identified by anomalous specific ionization energy loss in the ATLAS
Pixel detector. Gluino R-hadrons with lifetimes above 0.4 ns are excluded at 95% C.L. with lower mass limit range between 740 GeV and 1590 GeV. In the case of stable R-hadrons, the lower mass limit is 1570 GeV. See their Figs. 5 and 6.

14 KHACHATRYAN 16BW searched in 2.5 fb⁻¹ of pp collisions at √s = 13 TeV for events with heavy stable charged particles, identified by their anomalously high energy deposits in the silicon tracker and/or long time-of-flight measurements by the muon system. No evidence for an excess over the expected background is observed. Limits are derived for pair production of gluinos as a function of mass, depending on the interaction model and on the fraction f, of produced gluinos hadronizing into a g̃ - gluon state, see Fig. 4 and Table 7.

15 AAD 15AE searched in 19.1 fb⁻¹ of pp collisions at √s = 8 TeV for heavy long-lived charged particles, measured through their specific ionization energy loss in the ATLAS pixel detector or their time-of-flight in the ALTAS muon system. In the absence of an excess of events above the expected backgrounds, limits are set R-hadrons in various scenarios, see Fig. 11. Limits are also set in LeptoSUSY models where the gluino decays to stable 300 GeV leptons, see Fig. 9.

16 AAD 15BM searched in 18.4 fb⁻¹ of pp collisions at √s = 8 TeV for stable and metastable non-relativistic charged particles through their anomalous specific ionization energy loss in the ATLAS pixel detector. In absence of an excess of events above the expected backgrounds, limits are set within a generic R-hadron model, on stable gluino R-hadrons (see Table 5) and on metastable gluino R-hadrons decaying to (g̃ / q̃q̃) plus a light χ̃₁ (see Fig. 7) and decaying to tT plus a light χ̃₀ (see Fig. 9).

17 KHACHATRYAN 15AK looked in a data set corresponding to 18.6 fb⁻¹ of pp collisions at √s = 8 TeV, and a search interval corresponding to 281 h of trigger lifetime, for long-lived particles that have stopped in the CMS detector. No evidence for an excess over the expected background in a cloud interaction model is observed. Assuming the decay g̃ → gχ̃₀ and lifetimes between 1 µs and 1000 s, limits are derived on g̃ production as a function of m̃χ̃₀, see Figs. 4 and 6. The exclusions require that m̃χ̃₀ is kinematically consistent with the minimum values of the jet energy thresholds used.

18 AAD 13AA searched in 4.7 fb⁻¹ of pp collisions at √s = 7 TeV for events containing long-lived particles that hadronize forming R-hadrons. No significant excess above the expected background was found. Long-lived R-hadrons containing a g̃ are excluded for masses up to 985 GeV at 95% C.L in a general interaction model. Also, limits independent of the fraction of R-hadrons that arrive charged in the muon system were derived, see Fig. 6.

19 AAD 13BC searched in 5.0 fb⁻¹ of pp collisions at √s = 7 TeV and in 22.9 fb⁻¹ of pp collisions at √s = 8 TeV for bottom squark R-hadrons that have come to rest within the ATLAS calorimeter and decay at some later time to hadronic jets and a neutralino. In absence of an excess of events above the expected backgrounds, limits are set on gluino masses for different decays, lifetimes, and neutralino masses, see their Table 6 and Fig. 10.

20 CHATRYCHAN 13AB looked in 5.0 fb⁻¹ of pp collisions at √s = 7 TeV and in 18.8 fb⁻¹ of pp collisions at √s = 8 TeV for events with heavy stable particles, identified by their anomalous dE/dx in the tracker or additionally requiring that it be identified as muon in the muon chambers, from pair production of g̃'s. No evidence for an excess over the expected background is observed. Limits are derived for pair production of gluinos as a function of mass (see Fig. 8 and Table 5), depending on the fraction, f, of formation of g̃ - g̃ (R-gluonball) states. The quoted limit is for f = 0.1, while for f = 0.5 it degrades to 1276 GeV. In the conservative scenario where every hadronic interaction causes it to become neutral, the limit decreases to 928 GeV for f = 0.1.

21 AAD 12P looked in 31 pb⁻¹ of pp collisions at √s = 7 TeV for events with pair production of long-lived gluinos. The hadronization of the gluinos leads to R-hadrons which may stop inside the detector and later decay via g̃ → gχ̃₀ during gaps between the proton bunches. No significant excess over the expected background is observed. From a counting experiment, a limit at 95% C.L. on the cross section as a function of m̃g̃ is derived for m̃χ̃₀ = 100 GeV, see Fig. 4. The limit is valid for lifetimes between 10⁻⁵ and 10³ seconds and assumes the Generic matter interaction model for the production cross section.

22 CHATRYCHAN 12AN looked in 4.0 fb⁻¹ of pp collisions at √s = 7 TeV for events with pair production of long-lived gluinos. The hadronization of the gluinos leads to R-hadrons which may stop inside the detector and later decay via g̃ → gχ̃₀ during gaps between the proton bunches. No significant excess over the expected background is observed. From a counting experiment, a limit at 95% C.L. on the cross section as a function of m̃g̃ is derived, see Fig. 3. The mass limit is valid for lifetimes between 10⁻⁵ and 10³ seconds, for what they call "the daughter gluino energy E_g̃ >" 100 GeV and assuming the cloud interaction model for R-hadrons. Supersedes KHACHATRYAN 11.

23 CHATRYCHAN 12L looked in 5.0 fb⁻¹ of pp collisions at √s = 7 TeV for events with heavy stable particles, identified by their anomalous dE/dx in the tracker or additionally requiring that it be identified as muon in the muon chambers, from pair production of g̃'s. No evidence for an excess over the expected background is observed. Limits are derived for pair production of gluinos as a function of mass (see Fig. 3), depending on the fraction, f, of formation of g̃ - g̃ (R-gluoball) states. The quoted limit is for f = 0.1, while for f = 0.5 it degrades to 1046 GeV. In the conservative scenario where every hadronic interaction causes it to become neutral, the limit decreases to 928 GeV for f=0.1. Supersedes KHACHATRYAN 11C.

24 AAD 11k looked in 34 pb⁻¹ of pp collisions at √s = 7 TeV for events with heavy stable particles, identified by their anomalous dE/dx in the tracker or time of flight in the tile calorimeter, from pair production of g̃. No evidence for an excess over the SM expectation is observed. Limits are derived for pair production of gluinos as a function of mass (see Fig. 4), for a fraction, f = 10%, of formation of g̃ - g̃ (R-gluonball). If instead of a phase space driven approach for the hadronic scattering of the R-hadrons, a triple-Regge model or a bag-model is used, the limit degrades to 566 and 562 GeV, respectively.

25 AAD 11p looked in 37 pb⁻¹ of pp collisions at √s = 7 TeV for events with heavy stable particles, reconstructed and identified by their time of flight in the Muon System. There is no requirement on their observation in the tracker to increase the sensitivity to cases where gluinos have a large fraction, f, of formation of neutral g̃ - g̃ (R-gluonball). No evidence for an excess over the SM expectation is observed. Limits are derived as a function of mass (see Fig. 4), for f=0.1. For fractions f = 0.5 and 1.0 the limit degrades to 537 and 530 GeV, respectively.

26 KHACHATRYAN 11 looked in 10 pb⁻¹ of pp collisions at √s = 7 TeV for events with pair production of long-lived gluinos. The hadronization of the gluinos leads to R-hadrons which may stop inside the detector and later decay via g̃ → gχ̃₀ during gaps between the proton bunches. No significant excess over the expected background is observed.

From a counting experiment, a limit at 95% C.L. on the cross section times branching ratio is derived for m̃g̃ - m̃χ̃₀ > 100 GeV, see their Fig. 2. Assuming 100% branching

ratio, lifetimes between 75 ns and 3 × 10⁵ s are excluded for m̃g̃ = 300 GeV. The g̃ mass exclusion is obtained with the same assumptions for lifetimes between 10 µs and 1000 s, but shows some dependence on the model for R-hadron interactions with matter, illustrated in Fig. 3. From a time-profile analysis, the mass exclusion is 382 GeV for a lifetime of 10 µs under the same assumptions as above.

27 KHACHATRYAN 11c looked in 3.1 pb⁻¹ of pp collisions at √s = 7 TeV for events with heavy stable particles, identified by their anomalous dE/dx in the tracker or additionally requiring that it be identified as muon in the muon chambers, from pair production of g̃. No evidence for an excess over the expected background is observed. Limits are derived for pair production of gluinos as a function of mass (see Fig. 3), depending on the fraction, f, of formation of g̃ - g̃ (R-gluonball). The quoted limit is for f=0.1, while for f=0.5 it degrades to 357 GeV. In the conservative scenario where every hadronic interaction causes it to become neutral, the limit decreases to 311 GeV for f=0.1.

Light g̃ (Gravitino) mass limits from collider experiments

The following are bounds on light ( < ∼ 1 eV) gravitino indirectly inferred from its coupling to matter suppressed by the gravitino decay constant.

Unless otherwise stated, all limits assume that other supersymmetric particles besides the gravitino are too heavy to be produced. The gravitino is assumed to be undetected and to give rise to a missing energy (Ẽ) signature.

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

<table><thead><tr><th>VALUE (eV)</th><th>CL<sup>5</sup></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&bull; &bull; &bull; We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td>&bull; &bull; &bull;</td></tr><tr><td>&gt; 3.5 &times; 10<sup>-4</sup></td><td>95</td><td>1 AAD</td><td>15BH ATLS</td><td>jet + E<sub>T</sub>, pp &rarr; (g̃/g̃)g̃, m̃g̃ = m̃g̃ = 500 GeV</td></tr><tr><td>&gt; 3 &times; 10<sup>-4</sup></td><td>95</td><td>1 AAD</td><td>15BH ATLS</td><td>jet + E<sub>T</sub>, pp &rarr; (g̃/g̃)g̃, m̃g̃ = m̃g̃ = 1000 GeV</td></tr><tr><td>&gt; 2 &times; 10<sup>-4</sup></td><td>95</td><td>1 AAD</td><td>15BH ATLS</td><td>jet + E<sub>T</sub>, pp &rarr; (g̃/g̃)g̃, m̃g̃ = m̃g̃ = 1500 GeV</td></tr><tr><td>&gt; 1.09 &times; 10<sup>-5</sup></td><td>95</td><td>2 ABDALLAH</td><td>05B DLPH</td><td>e<sup>+</sup>e<sup>-</sup> &rarr; g̃g̃γ</td></tr><tr><td>&gt; 1.35 &times; 10<sup>-5</sup></td><td>95</td><td>3 ACHARD</td><td>04E L3</td><td>e<sup>+</sup>e<sup>-</sup> &rarr; g̃g̃γ</td></tr><tr><td>&gt; 1.3 &times; 10<sup>-5</sup></td><td>95</td><td>4 HEISTER</td><td>03C ALEP</td><td>e<sup>+</sup>e<sup>-</sup> &rarr; g̃g̃γ</td></tr><tr><td>&gt; 11.7 &times; 10<sup>-6</sup></td><td>95</td><td>5 ACOSTA</td><td>02H CDF</td><td>p̃p̃ &rarr; g̃g̃γ</td></tr><tr><td>&gt; 8.7 &times; 10<sup>-6</sup></td><td>95</td><td>6 ABIENDI,G</td><td>00D OPAL</td><td>e<sup>+</sup>e<sup>-</sup> &rarr; g̃g̃γ</td></tr></tbody></table>

1 AAD 15BH searched in 20.3 fb⁻¹ of pp collisions at √s = 8 TeV for associated production of a light gravitino and a squark or gluino. The squark (gluino) is assumed to decay exclusively to a quark (gluon) and a gravitino. No evidence was found for an excess above the expected level of Standard Model background and 95% C.L. lower limits were set on the gravitino mass as a function of the squark/gluino mass, both in the case of degenerate and non-degenerate squark/gluino masses, see Figs. 14 and 15.

2 ABDALLAH 05B use data from √s = 180–208 GeV. They look for events with a single photon + Ẽ final states from which a cross section limit of σ < 0.18 pb at 208 GeV is obtained, allowing a limit on the mass to be set. Supersedes the results of ABREU 00Z.

3 ACHARD 04E use data from √s = 189–209 GeV. They look for events with a single photon + Ẽ final states from which a limit on the Gravitino mass is set corresponding to √F > 238 GeV. Supersedes the results of ACCIARRI 99R.

4 HEISTER 03C use the data from √s = 189–209 GeV to search for γẼT final states.

5 ACOSTA 02H looked in 87 pb⁻¹ of p̃p̃ collisions at √s = 1.8 TeV for events with a high-ẼT photon and ẼT. They compared the data with a GMSB model where the final state could arise from q̃q̃ → g̃g̃γ. Since the cross section for this process scales as 1/|F|⁴, a limit at 95% CL is derived on |F|¹/² > 221 GeV. A model independent limit for the above topology is also given in the paper.

6 ABIENDI,G 00D searches for γẼ final states from √s = 189 GeV.

Supersymmetry miscellaneous results

Results that do not appear under other headings or that make nonminimal assumptions.

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

<table><thead><tr><th>VALUE</th><th>CL<sup>5</sup></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&bull; &bull; &bull; We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td>&bull; &bull; &bull;</td></tr><tr><td>none 450-1400</td><td>95</td><td>1 AAD</td><td>20C ATLS</td><td>habemus MSSM, m<sub>A</sub>-tan&beta; plane</td></tr><tr><td></td><td></td><td>2 AAD</td><td>20L ATLS</td><td>heavy neutral Higgs bosons, hMSSM, m<sub>A</sub>-tan&beta; plane</td></tr><tr><td>&gt;65</td><td>95</td><td>3 AABOUD</td><td>16AF ATLS</td><td>selected ATLAS searches on EWK sector</td></tr><tr><td>none 0-2</td><td>95</td><td>4 AAD</td><td>16AG ATLS</td><td>dark photon, &gamma;<sub>d</sub>, in SUSY- and Higgs-portal models</td></tr><tr><td></td><td></td><td>5 AAD</td><td>13P ATLS</td><td>dark &gamma;, hidden valley</td></tr><tr><td></td><td></td><td>6 AALTONEN</td><td>12AB CDF</td><td>hidden-valley Higgs</td></tr><tr><td></td><td></td><td>7 AAD</td><td>11AA ATLS</td><td>scalar gluons</td></tr><tr><td>none 100-185</td><td>95</td><td>8 CHATRYCHAN11E CMS</td><td>&mu;&mu; resonances</td><td></td></tr><tr><td></td><td></td><td>9 ABAZOV</td><td>10N D0</td><td>&gamma;D, hidden valley</td></tr></tbody></table>

1 AAD 20C uses a statistical combination of six final states b̃b̃b̃, b̃bWW, b̃bττ, WWWW, b̃bγγ, and WWγγ to search for non-resonant and resonant production of Higgs boson pairs. The search uses 36.1 fb⁻¹ of pp collisions data at √s = 13 TeV. Constraints in the habemus Minimal Supersymmetric Standard Model in the (m<sub>A</sub>, tan&beta;) parameter space are placed, see their Figure 7(b).

2 AAD 20L used 27.8 fb⁻¹ of pp collision data at √s = 13 TeV to search for heavy neutral Higgs bosons produced in association with at least one b-quark and decaying into a pair
of b-quarks. The data are compatible with SM expectations, yielding no significant excess of events in the mass range 450-1400 GeV, see their Fig. 11. Exclusion limits at 95% C.L. were derived in hMSSM scenarios as a function of $m_A$ and $\tan\beta$, see their Fig. 9 and 10.

3 AABOUD 16AF uses a selection of searches by ATLAS for the electroweak production of SUSY particles studying resulting constraints on dark matter candidates. They use $20 \text{ fb}^{-1}$ of $pp$ collisions at $\sqrt{s} = 8$ TeV. A likelihood-driven model of an effective model focusing on the gaugino-higgsino and Higgs sector of the pMSSM is performed. The ATLAS searches impact models where $m_{\chi_1^0} < 65$ GeV, excluding 86% of them. See

their Figs. 2, 4, and 6.

4 AAD 16AG searches for prompt lepton-jets using $20 \text{ fb}^{-1}$ of $pp$ collisions at $\sqrt{s} = 8$ TeV collected with the ATLAS detector. Lepton-jets are expected from decays of low-mass dark photons in SUSY-portal and Higgs-portal models. No significant excess of events is observed and 95% CL upper limits are computed on the production cross section times branching ratio for two prompt lepton-jets in models predicting 2 or 4 $\gamma$ via SUSY-portal topologies, for $\gamma_d$ mass values between 0 and 2 GeV. See their Figs 9 and 10. The results are also interpreted in terms of a 90% CL exclusion region in kinetic mixing and dark-photon mass parameter space. See their Fig. 13.

5 AAD 13P searched in $5 \text{ fb}^{-1}$ of $pp$ collisions at $\sqrt{s} = 7$ TeV for single lepton-jets with at least four muons; pairs of lepton-jets, each with two or more muons; and pairs of lepton-jets with two or more electrons. All of these could be signatures of Hidden Valley supersymmetric models. No statistically significant deviations from the Standard Model expectations are found. 95% C.L. limits are placed on the production cross section times branching ratio of dark photons for several parameter sets of a Hidden Valley model.

6 AALTONEN 12AB looked in $5 \text{ fb}^{-1}$ of $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV for anomalous production of multiple low-energy leptons in association with a $W$ or $Z$ boson. Such events may occur in hidden valley models in which a supersymmetric Higgs boson is produced in association with a $W$ or $Z$ boson, with $H \to \chi_1^0 \chi_1^0$ pair and with the $\chi_1^0$ further decaying into a dark photon ($\gamma_D$) and the unobservable lightest SUSY particle of the hidden sector. As the $\gamma_D$ is expected to be light, it may decay into a lepton pair. No significant excess over the SM expectation is observed and a limit at 95% C.L. is set on the cross section for a benchmark model of supersymmetric hidden-valley Higgs production.

7 AAD 11AA looked in $34 \text{ pb}^{-1}$ of $pp$ collisions at $\sqrt{s} = 7$ TeV for events with $\ge 4$ jets originating from pair production of scalar gluons, each decaying to two gluons. No two-jet resonances are observed over the SM background. Limits are derived on the cross section times branching ratio (see Fig. 3). Assuming 100% branching ratio for the decay to two gluons, the quoted exclusion range is obtained, except for a 5 GeV mass window around 140 GeV.

8 CHATRYCHAN 11E looked in $35 \text{ pb}^{-1}$ of $pp$ collisions at $\sqrt{s} = 7$ TeV for events with collimated $\mu$ pairs (leptonic jets) from the decay of hidden sector states. No evidence for new resonance production is found. Limits are derived and compared to various SUSY models (see Fig. 4) where the LSP, either the $\chi_1^0$ or a $\tilde{q}$, decays to dark sector particles.

9 ABAZOV 10N looked in $5.8 \text{ fb}^{-1}$ of $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV for events from hidden valley models in which a $\chi_1^0$ decays into a dark photon, $\gamma_D$, and the unobservable lightest SUSY particle of the hidden sector. As the $\gamma_D$ is expected to be light, it may decay into a tightly collimated lepton pair, called lepton pair. They searched for events with $E_T$ and two isolated lepton jets observable by an opposite charged lepton pair e, $e\mu$ or $\mu\mu$. No significant excess over the SM expectation is observed, and a limit at 95% C.L. on the cross section times branching ratio is derived, see their Table I. They also examined the invariant mass of the lepton jets for a narrow resonance, see their Fig. 4, but found no evidence for a signal.

REFERENCES FOR Supersymmetric Particle Searches

<table><tbody><tr><td>AAD</td><td>23AB JHEP 2307 021</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23AE EPJ C83 515</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23AL EPJ C83 561</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23AR PR D108 012012</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23BQ PL B846 138172</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23CB JHEP 2310 082</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23CI JHEP 2312 167</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23CP JHEP 2311 150</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23CR JHEP 2312 081</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23D JHEP 2306 158</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>23M JHEP 2307 031</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AALBERS</td><td>23 PRL 131 041002</td><td>J. Aalbers et al.</td><td>(LZ Collab.)</td></tr><tr><td>ABE</td><td>23 PRL 130 061002</td><td>H. Abe et al.</td><td>(MAGIC Collab.)</td></tr><tr><td>APRILE</td><td>23A PRL 131 041003</td><td>E. Aprile et al.</td><td>(XENONnT Collab.)</td></tr><tr><td>FOSTER</td><td>23 PRL D107 103047</td><td>J.W. Foster et al.</td><td>(PANDA-4T Collab.)</td></tr><tr><td>GUO</td><td>23A PRL D108 043001</td><td>X.-K. Guo et al.</td><td>(PANDA-4T Collab.)</td></tr><tr><td>HAYRAPETY...</td><td>23E JHEP 2310 046</td><td>A. Hayrapetyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>LEES</td><td>23E PRL 131 020181</td><td>J.P. Lees et al.</td><td>(BABAR Collab.)</td></tr><tr><td>TUMASYAN</td><td>23AB JHEP 2307 110</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23C PR D108 012011</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23AO JHEP 2307 210</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23AY JHEP 2309 149</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23B PL B842 137460</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23H JHEP 2305 227</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23K JHEP 2306 060</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23L JHEP 2307 161</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23X EPJ C83 571</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>22E PL B830 137106</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>22U EPJ C82 606</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>ABBASI</td><td>22B PR D105 062004</td><td>R. Abbasi et al.</td><td>(IceCube Collab.)</td></tr><tr><td>ABDALLA</td><td>22 H. Aad et al.</td><td>H. Abdalla et al.</td><td>(PANDA-4T Collab.)</td></tr><tr><td>HUANG</td><td>22 PL B834 137487</td><td>Z. Huang et al.</td><td>(PANDA-4T Collab.)</td></tr><tr><td>TUMASYAN</td><td>22AF EPJ C82 153</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22Q JHEP 2204 091</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22S JHEP 2204 147</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22V PR D104 02014</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>21AK EPJ C81 600</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21AL PRL 127 059182</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21AM PR D104 032014</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21AW PR D104 112005</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21AX PR D104 112010</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21B EPJ C81 11</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>Also</td><td>21Bf EPJ C81 1023</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21BG EPJ C81 1118</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21E PR D103 112003</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21F PR D103 112006</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21L JHEP 2102 143</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21O JHEP 2104 174</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21P JHEP 2104 165</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21S JHEP 2105 093</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr></tbody></table>

<table><tbody><tr><td>AAD</td><td>21X JHEP 2107 173</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21Y JHEP 2107 167</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAIJ</td><td>21Z PRL C81 261</td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr><tr><td>ABDALLAH</td><td>21 PR D103 102002</td><td>H. Abdallah et al.</td><td>(H.E.S.S. Collab.)</td></tr><tr><td>MENG</td><td>21B PRL 127 261802</td><td>Y. Meng et al.</td><td>(PANDA-4T Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21AD PR D104 052001</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21AF PR D104 052011</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21B EPJ C81 3</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21M JHEP 2104 123</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21U PR D104 012015</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21V PR D104 032006</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>21C JHEP 2110 045</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>21I EPJ C81 970</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AABOUD</td><td>20 EPJ C80 754</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20AL JHEP 2010 062</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20AN JHEP 2010 005</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20AS JHEP 2010 1080</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20B PL B800 135103</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20D PL B801 135114</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20H PR D101 032009</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20I PR D101 052005</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20K PR D101 072001</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20L PR D101 032004</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20M PR D102 032006</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20O EPJ C80 123</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20R EPJ C80 691</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20S EPJ C80 737</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20T PR D102 006201</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>ABAZAJIAN</td><td>20 PR D102 043012</td><td>K.N. Abdazajan et al.</td><td>(UCI, VPI, TOKY+)</td></tr><tr><td>ABDALLAH</td><td>20 PR D102 062001</td><td>H. Abdallah et al.</td><td>(H.E.S.S. Collab.)</td></tr><tr><td>ABE</td><td>20G PR D102 072002</td><td>K. Abe et al.</td><td>(Super-Kamiokande Collab.)</td></tr><tr><td>ALBERT</td><td>20P PR D101 103001</td><td>A. Albert et al.</td><td>(HAWC Collab.)</td></tr><tr><td>ALBERT</td><td>20A PR B805 135439</td><td>A. Albert et al.</td><td>(ANTARES Collab.)</td></tr><tr><td>ALBERT</td><td>20C PR D102 008202</td><td>A. Albert et al.</td><td>(ANTARES and IceCube Collab.)</td></tr><tr><td>ALVAREZ</td><td>20J CJP 2009 004</td><td>A. Albert et al.</td><td>(ANTARES and IceCube Collab.)</td></tr><tr><td>HOOF</td><td>20 JHEP 2002 012</td><td>S. Hoof, A. Geringer-Sameth, R. Trotta</td><td>(GOET+)</td></tr><tr><td>SIRUNYAN</td><td>20AH JHEP 2005 032</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20AU PRL 124 041803</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20AF PR D104 135183</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20BJ JHEP 2009 149</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20E PR D101 052010</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20F PL B806 135502</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20P EPJ C80 189</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20S JHEP 2006 752</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20T JHEP 2002 015</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>WANG</td><td>20G CP C44 125001</td><td>Q. Wang et al.</td><td>(PANDA-II Collab.)</td></tr><tr><td>AABOUD</td><td>19AT PR D99 092007</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19AU PR D100 012006</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19C PL B788 96</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19D PL D102 012001</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>19I PR D99 012009</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>19H JHEP 1912 060</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>ABE</td><td>19 PL B789 45</td><td>K. Abe et al.</td><td>(XMASS Collab.)</td></tr><tr><td>AJAJ</td><td>19 PR D100 022004</td><td>R. Ajaj et al.</td><td>(DEAP-3600 Collab.)</td></tr><tr><td>ARULE</td><td>19P PR D100 022001</td><td>C. Amok et al.</td><td>(PICO Collab.)</td></tr><tr><td>APRILE</td><td>19A PRL 122 141301</td><td>E. Aprile et al.</td><td>(XENON1T Collab.)</td></tr><tr><td>DI-MAURO</td><td>19A PR D99 123027</td><td>M. Di Mauro et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>JOHNSON</td><td>19D PR D99 103007</td><td>C. Johnson et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>LI</td><td>19 PR D99 123519</td><td>S. Li et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19AG JHEP 1906 143</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19AO EPJ C79 305</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19AU EPJ C79 444</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19AW PL B790 140</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19BH PR D99 032011</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19BI PR D99 032014</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19BJ PR D99 052002</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19BT PL B797 134876</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19BU JHEP 1908 150</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19CA PR D100 112003</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19CE PRL 123 241801</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19CH JHEP 1910 244</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19CI JHEP 1911 109</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19F PR D99 012010</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19K JHEP 1901 154</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19S JHEP 1903 031</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19U JHEP 1903 101</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>XIA</td><td>19A PL B792 193</td><td>J. Xia et al.</td><td>(PANDA-II Collab.)</td></tr><tr><td>AABOUD</td><td>18AQ JHEP 1806 108</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18AP JHEP 1806 107</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18AS JHEP 1806 022</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18AY EPJ C78 154</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18BB EPJ C78 250</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18BJ EPJ C78 625</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18BT JHEP C78 995</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18BV JHEP 1809 050</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18CF PL B785 136</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18CB PR D98 092002</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18CM PR D98 092008</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18CO PR D98 092012</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18I JHEP 1801 126</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18P PR D97 032003</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18R PR D97 052010</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18U PR D97 092006</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18V PR D97 112001</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18W PR D98 032008</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18Z PR D98 032009</td><td>M. Aaboud et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>ABDALLAH</td><td>18Z PR D102 1201101</td><td>H. Abdallah et al.</td><td>(H.E.S.S. Collab.)</td></tr><tr><td>ADHIKARI</td><td>18N SAT 64 83</td><td>A. Adhikari et al.</td><td>(COSINE-100 Collab.)</td></tr><tr><td>AGNES</td><td>18A PR D98 102006</td><td>P. Agnes et al.</td><td>(DarkSide-50 Collab.)</td></tr><tr><td>AGNESE</td><td>18A PRL 120 061802</td><td>R. Agnese et al.</td><td>(SuperCDMS Collab.)</td></tr><tr><td>AHNEN</td><td>18 JCAP 1803 009</td><td>M.L. Ahnen et al.</td><td>(MAGIC Collab.)</td></tr><tr><td>AHLAW</td><td>18C JCAP 1806 043</td><td>A. Ahlaw et al.</td><td>(HAWC Collab.)</td></tr><tr><td>ALBERT</td><td>18C PR D98 123012</td><td>A. Albert et al.</td><td>(HAWC Collab.)</td></tr><tr><td>AMAUDRUZ</td><td>18 PRL 121 071801</td><td>P.A. Amaudruz et al.</td><td>(DEAP-3600 Collab.)</td></tr><tr><td>APRILE</td><td>18 PRL 121 111302</td><td>E. Aprile et al.</td><td>(XENON1T Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AA PL B780 118</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AC PL B780 384</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AD PL B780 432</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AJ PL B782 440</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AK PL B783 114</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AL JHEP 1802 067</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AN JHEP 1803 167</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AO JHEP 1803 166</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AP JHEP 1803 160</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AR JHEP 1803 076</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18AT JHEP 1804 073</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18B PL B788 263</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18BR JHEP 1808 016</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18C PR D97 032009</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18D PR D97 012007</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr></tbody></table>
# Searches Particle Listings

## Supersymmetric Particle Searches

<table><tbody><tr><td>ANGLOHER</td><td>12</td><td>EPJ C72 1971</td><td>G. Angloher et al.</td><td>(CRESST-II Collab.)</td></tr><tr><td>APRILE</td><td>12</td><td>PRL 109 181301</td><td>E. Aprile et al.</td><td>(XENON100 Collab.)</td></tr><tr><td>ARBEY</td><td>12</td><td>PL B708 162</td><td>A. Arbey et al.</td><td></td></tr><tr><td>ARCHAMBAU</td><td>12</td><td>PL B711 153</td><td>S. Archambault et al.</td><td>(PICASSO Collab.)</td></tr><tr><td>BAER</td><td>12</td><td>EPJ 1205 091</td><td>H. Baer, V. Barger, A. Mustafayev</td><td>(OKLA, WISC+)</td></tr><tr><td>BALAZS</td><td>12</td><td>EPJ C73 2563</td><td>C. Balazs et al.</td><td></td></tr><tr><td>BEDCHLE</td><td>12</td><td>PL B706 098</td><td>J. Benthle et al.</td><td></td></tr><tr><td>BEHNKE</td><td>12</td><td>PR D86 052001</td><td>E. Behnke et al.</td><td>(COUPP Collab.)</td></tr><tr><td>Also</td><td></td><td>PR D90 079902 (errat.)</td><td>E. Behnke et al.</td><td>(COUPP Collab.)</td></tr><tr><td>BESKIDT</td><td>12</td><td>EPJ C72 2166</td><td>C. Beskidt et al.</td><td>(KARLE, JINR, ITEP)</td></tr><tr><td>BOTTINO</td><td>12</td><td>PR D85 095013</td><td>A. Bottino, N. Fornengo, S. Scopel</td><td>(TORI, SOGA)</td></tr><tr><td>BOWMUEL</td><td>12</td><td>PL D70 2020</td><td>H. Suchmuller et al.</td><td></td></tr><tr><td>CAO</td><td>12A</td><td>PL B710 665</td><td>J. Cao et al.</td><td></td></tr><tr><td>CHATRYAN</td><td>12</td><td>PR D85 081204</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYAN</td><td>12AE</td><td>PRL 109 171803</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYAN</td><td>12AI</td><td>EPJHEP 1208 110</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHAZKAN</td><td>12AI</td><td>PL B711 1206 169</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHAZKAN</td><td>12AN</td><td>EPJHEP 1208 026</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHAZKAN</td><td>12AT</td><td>EPJHEP 1210 018</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHAZKAN</td><td>12BJ</td><td>EPJHEP 1211 147</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHAZKAN</td><td>12BK</td><td>EPJHEP 1211 172</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHAZKAN</td><td>12BO</td><td>EPJHEP 1212 055</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHAZKAN</td><td>12CL</td><td>PL B710 408</td><td>E. Daw et al.</td><td>(DRIFT-IID Collab.)</td></tr><tr><td>DAW</td><td>12</td><td>ASP 35 397</td><td>H.K. Dreiner, M. Kramer, J. Tattersall</td><td>(BONN+)</td></tr><tr><td>DREINER</td><td>12A</td><td>EPJ 99 61001</td><td>J. Ellis, K. Olive</td><td></td></tr><tr><td>ELLIS</td><td>12B</td><td>EPJ C72 2005</td><td>M. Felizardo et al.</td><td>(SIMPLE Collab.)</td></tr><tr><td>FELIZARDO</td><td>12B</td><td>PRL 108 201302</td><td>J. Feng, K. Matchev, D. Sanford</td><td></td></tr><tr><td>FENK</td><td>12B</td><td>PR D85 075007</td><td>M. Kadastik et al.</td><td></td></tr><tr><td>KADASTIK</td><td>12</td><td>EPJHEP 1205 061</td><td>S.C. Kim et al.</td><td>(KIMS Collab.)</td></tr><tr><td>KIM</td><td>12</td><td>PRL 108 181301</td><td>C. Strege et al.</td><td>(LOIC, AMST, MADU, GRAN+)</td></tr><tr><td>STREGE</td><td>12</td><td>JCAP 1203 030</td><td>G. Strege et al.</td><td></td></tr><tr><td>AAD</td><td>11Aa</td><td>PL B71 C 182</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>11G</td><td>PL 106 131802</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>11K</td><td>PL B701 1</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>11O</td><td>PL B701 398</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>11P</td><td>PL B703 428</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>11Z</td><td>EPJ C71 1809</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AHMED</td><td>11Aa</td><td>PL B702 329</td><td>Z. Ahmed et al.</td><td>(CDMS and EDELWEISS-I Collab.)</td></tr><tr><td>ARMENGAUD</td><td>11</td><td>EPJ C71 1583</td><td>O. Buchmueller et al.</td><td></td></tr><tr><td>BUCHMUEL</td><td>11B</td><td>EPJ C71 1722</td><td>O. Buchmueller et al.</td><td></td></tr><tr><td>CHATRYAN</td><td>11B</td><td>EPJHEP 1106 093</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYAN</td><td>11C</td><td>PL B711 113</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYAN</td><td>11E</td><td>EPJHEP 1107 098</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYAN</td><td>11V</td><td>PL B704 411</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHACHATRY</td><td>11C</td><td>PR 106 011801</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHACHATRY</td><td>11C</td><td>EPJHEP 1103 024</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>ROSKOWSKI</td><td>11C</td><td>PR D83 015014</td><td>L. Roskowski et al.</td><td></td></tr><tr><td>ALTONEN</td><td>11C</td><td>PL D84 011801</td><td>L. Altonen et al.</td><td>(CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>10R</td><td>PR 105 081802</td><td>T. Altonen et al.</td><td></td></tr><tr><td>AALTONEN</td><td>10R</td><td>PR 105 191801</td><td>T. Altonen et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABAZOV</td><td>10L</td><td>PL B693 95</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ABAZOV</td><td>10M</td><td>PR 105 191802</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ABAZOV</td><td>10N</td><td>PR 105 211802</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ABAZOV</td><td>10P</td><td>PR 105 221802</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ACRMANN</td><td>10</td><td>JCAP 1005 025</td><td>M. Ackermann</td><td>(Fermi-LAT Collab.)</td></tr><tr><td>ARMENGAUD</td><td>10</td><td>PL B687 294</td><td>E. Armengaud et al.</td><td>(EDELWEISS-II Collab.)</td></tr><tr><td>ALLIS</td><td>09M</td><td>EPJ C69 201</td><td>J. Ellis, A. Mustafayev, K. Olive</td><td></td></tr><tr><td>ABAZOV</td><td>09M</td><td>PR 102 161802</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>AHMED</td><td>09</td><td>ASP 102 011301</td><td>Z. Ahmed et al.</td><td>(CDMS Collab.)</td></tr><tr><td>ANGLOHER</td><td>09</td><td>PL A9 270</td><td>G. Angloher et al.</td><td>(CRESST Collab.)</td></tr><tr><td>BUCHMUEL</td><td>09</td><td>EPJ C64 391</td><td>O. Buchmueller et al.</td><td>(LOIC, FNAL, CERN+)</td></tr><tr><td>DREINER</td><td>09</td><td>EPJ C62 547</td><td>H. Dreiner et al.</td><td></td></tr><tr><td>LEBEDENKO</td><td>09A</td><td>PR D80 052010</td><td>V.N. Lebedenko et al.</td><td></td></tr><tr><td>LEBEDENKO</td><td>09A</td><td>PR D80 151302</td><td>V. Lebedenko et al.</td><td>(ZEPLIN-II Collab.)</td></tr><tr><td>SORENSEN</td><td>09A</td><td>NIM A601 339</td><td>P. Sorensen et al.</td><td>(XENON10 Collab.)</td></tr><tr><td>ABAZOV</td><td>08F</td><td>PL B659 856</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ANGLE</td><td>08</td><td>PRL 100 021303</td><td>J. Angle et al.</td><td>(XENON10 Collab.)</td></tr><tr><td>ANGLE</td><td>08A</td><td>PRL 101 091301</td><td>J. Angle et al.</td><td>(XENON10 Collab.)</td></tr><tr><td>BEDNYAKOV</td><td>08A</td><td>PL 76 111</td><td>V. Bednyakov, H.P. Klapdor-Kleingrothaus, I.V. Kriwosheina</td><td></td></tr><tr><td>BEHNKE</td><td>08</td><td>SCI 319 933</td><td>E. Behnke</td><td></td></tr><tr><td>BENETTI</td><td>08</td><td>ASP 28 495</td><td>P. Benetti et al.</td><td>(COUPP Collab.)</td></tr><tr><td>BUCHMUEL</td><td>08</td><td>EPJHEP 0809 117</td><td>O. Buchmueller et al.</td><td></td></tr><tr><td>ABULENCIA</td><td>07H</td><td>EPJHEP 98 131804</td><td>A. Abulencia et al.</td><td>(CERN, MINN)</td></tr><tr><td>ALNER</td><td>07A</td><td>ASP 28 287</td><td>G.J. Alner et al.</td><td></td></tr><tr><td>CALIBILI</td><td>07A</td><td>EPJHEP 0709 081</td><td>L. Calibli et al.</td><td></td></tr><tr><td>ELLIS</td><td>07A</td><td>EPJHEP 0706 079</td><td>J. Ellis, K. Olive, P. Sandick</td><td>(CERN, MINN)</td></tr><tr><td>ELLIS</td><td>07A</td><td>EPJHEP 0706 079</td><td>H.S. Lee et al.</td><td>(KIMS Collab.)</td></tr><tr><td>ABBIENDI</td><td>06B</td><td>EPJ C46 307</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ACHTERBERG</td><td>06</td><td>ASP 26 129</td><td>A. Achterberg et al.</td><td>(AMANDA Collab.)</td></tr><tr><td>ACCKERMANN</td><td>06</td><td>ASP 24 459</td><td>M. Ackermann et al.</td><td>(AMANDA Collab.)</td></tr><tr><td>AKERIB</td><td>06</td><td>PR D73 011102</td><td>D.S. Akerib et al.</td><td>(CDMS Collab.)</td></tr><tr><td>AKERIB</td><td>06A</td><td>PR D73 011102</td><td>D.S. Akerib et al.</td><td>(CDMS Collab.)</td></tr><tr><td>06A</td><td>PR D73 015013</td><td>A. Allanbach et al.</td><td></td></tr><tr><td>BENOIT</td><td>06</td><td>PL B637 156</td><td>A. Benoit et al.</td><td></td></tr><tr><td>DE-AUSTRI</td><td>06</td><td>EPJHEP 0605 002</td><td>R.R. de Austri, R. Trotta, L. Roszkowski</td><td></td></tr><tr><td>DEBERO</td><td>06</td><td>PL B636 135</td><td>W. de Boer et al.</td><td></td></tr><tr><td>LEP-SLC</td><td>06</td><td>PRPL 427 257</td><td>LEPH, DELPHI, L3, OPAL, SLD and working groups</td><td></td></tr><tr><td>SHIMIZU</td><td>06A</td><td>PL B633 195</td><td>Y. Shimizu et al.</td><td></td></tr><tr><td>SMITH</td><td>06</td><td>PL B642 567</td><td>N.J.T. Smith, A.S. Murphy, T.J. Summer</td><td></td></tr><tr><td>ABAZOV</td><td>06A</td><td>V.M. Abazov et al.</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ABDALLAH</td><td>05B</td><td>EPJ C38 395</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>AKERIB</td><td>05B</td><td>PR D72 052009</td><td>D.S. Akerib et al.</td><td>(CDMS Collab.)</td></tr><tr><td>ALNER</td><td>05</td><td>PL B70 17</td><td>G.J. Alner et al.</td><td>(UK Dark Matter Collab.)</td></tr><tr><td>ALNER</td><td>05A</td><td>ASP 23 444</td><td>H. Baer et al.</td><td>(FSU, MSU, HAWA)</td></tr><tr><td>BAER</td><td>05A</td><td>EPJHEP 0507 065</td><td>M. Barnabe-Heider et al.</td><td>(PICASSO Collab.)</td></tr><tr><td>BARNABE-HE...</td><td>05</td><td>PL B624 186</td><td></td><td></td></tr><tr><td>ELLIS</td><td>05</td><td>PR D71 095007</td><td>J. Ellis et al.</td><td></td></tr><tr><td>SANGLARD</td><td>05</td><td>EPJHEP 122002</td><td>V. Sanglard et al.</td><td>(EDELWEISS Collab.)</td></tr><tr><td>ABBIENDI</td><td>04</td><td>EPJ C33 149</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABBIENDI</td><td>04N</td><td>EPJ C35 1</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABBIENDI</td><td>04H</td><td>EPJ C35 167</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABDALLAH</td><td>04H</td><td>EPJ C34 145</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABDALLAH</td><td>04M</td><td>EPJ C34 145</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABDALLAH</td><td>04M</td><td>EPJ C37 129 (errat.)</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>Also</td><td></td><td></td><td></td><td></td></tr><tr><td>ACHARD</td><td>04E</td><td>PL B580 37</td><td>P. Achard et al.</td><td>(L3 Collab.)</td></tr><tr><td>ACHARD</td><td>04E</td><td>PL B587 16</td><td>P. Achard et al.</td><td>(L3 Collab.)</td></tr><tr><td>AKERIB</td><td>04</td><td>PRL 93 211301</td><td>D.S. Akerib et al.</td><td></td></tr><tr><td>04</td><td>PR D70 0410 052</td><td>Baltz, P. Gondolo</td><td></td></tr><tr><td>04</td><td>PR D70 0410 012</td><td>G. Belanger et al.</td><td></td></tr><tr><td>04</td><td>PR D70 0410 012</td><td>A. Böttino et al.</td><td></td></tr><tr><td>04</td><td>PR D70 0410 012</td><td>S. Desai et al.</td><td></td></tr><tr><td>04B</td><td>PR D70 055005</td><td>J. Ellis et al.</td><td></td></tr><tr><td>04</td><td>PR D70 055005</td><td>J. Ellis et al.</td><td></td></tr><tr><td>04</td><td>PR D70 055005</td><td>A. Heister et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>04A</td><td>PR D70 075006</td><td>A. Pierce</td><td></td></tr><tr><td>ABBIENDI</td><td>04L</td><td>PL B572 8</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABDALLAH</td><td>03M</td><td>EPJ C31 421</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr></tbody></table>

<table><tbody><tr><td>AHMED</td><td>03</td><td>ASP 19 691</td><td>B. Ahmed et al.</td><td>(UK Dark Matter Collab.)</td></tr><tr><td>AKERIB</td><td>03</td><td>PR D68 082002</td><td>D.S. Akerib et al.</td><td>(CDMS Collab.)</td></tr><tr><td>BAER</td><td>03</td><td>JCAP 0305 006</td><td>H. Baer, C. Balazs</td><td></td></tr><tr><td>BAER</td><td>03A</td><td>JCAP 0309 007</td><td>H. Baer et al.</td><td></td></tr><tr><td>BOTTINO</td><td>03</td><td>PR D68 043506</td><td>A. Bottino et al.</td><td></td></tr><tr><td>BOTTINO</td><td>03A</td><td>PR D67 063519</td><td>A. Bottino, N. Fornengo, S. Scopel</td><td></td></tr><tr><td>CHATTOPAD...</td><td>03</td><td>PR D68 035005</td><td>U. Chattopadhyay, A. Corsetti, P. Nath</td><td></td></tr><tr><td>ELLIS</td><td>03</td><td>ASP 18 395</td><td>J. Ellis, K.A. Olive, Y. Santoso</td><td></td></tr><tr><td>ELLIS</td><td>03B</td><td>NP B652 259</td><td>J. Ellis et al.</td><td></td></tr><tr><td>ELLIS</td><td>03C</td><td>PL B565 176</td><td>J. Ellis et al.</td><td></td></tr><tr><td>ELLIS</td><td>03D</td><td>PL B573 162</td><td>J. Ellis et al.</td><td></td></tr><tr><td>ELLIS</td><td>03E</td><td>PR D70 123502</td><td>J. Ellis et al.</td><td></td></tr><tr><td>HEISTER</td><td>03C</td><td>EPJ C28 1</td><td>A. Heister et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>HEISTER</td><td>03G</td><td>EPJ C31 1</td><td>A. Heister et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>KLAPDOR-K...</td><td>03</td><td>ASP 18 525</td><td>H.V. Klapdor-Kleingrothaus et al.</td><td></td></tr><tr><td>LAHANAS</td><td>03</td><td>PL B568 55</td><td>A. Lahanas, D. Nanopoulos</td><td></td></tr><tr><td>TAKEDA</td><td>03</td><td>PL B572 145</td><td>A. Takeda et al.</td><td></td></tr><tr><td>ABRAMS</td><td>03A</td><td>PR D66 122003</td><td>D. Abrams et al.</td><td>(CDMS Collab.)</td></tr><tr><td>ACOSTA</td><td>02H</td><td>PRL 89 281801</td><td>D. Acosta et al.</td><td>(CDF Collab.)</td></tr><tr><td>ANGLOHER</td><td>02B</td><td>ASP 18 43</td><td>G. Angloher et al.</td><td>(CRESST Collab.)</td></tr><tr><td>ARNOWITT</td><td>02</td><td>hep-ph/0211417</td><td>R. Arnowitt, B. Dutta</td><td></td></tr><tr><td>ELLIS</td><td>02B</td><td>PL B532 318</td><td>J. Ellis, A. Ferstl, K.A. Olive</td><td>(ALEPH Collab.)</td></tr><tr><td>HEISTER</td><td>02C</td><td>PL B56 191</td><td>A. Heister et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>HEISTER</td><td>02E</td><td>PL B526 206</td><td>A. Heister et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>HEISTER</td><td>02E</td><td>PL B533 223</td><td>A. Heister et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>KIM</td><td>02N</td><td>PL B544 73</td><td>H.B. Kim et al.</td><td></td></tr><tr><td>KIM</td><td>02B</td><td>JHEP 0212 034</td><td>Y. Kim et al.</td><td></td></tr><tr><td>LAHANAS</td><td>02B</td><td>EPJ C23 185</td><td>A. Lahanas, V.C. Spanos</td><td></td></tr><tr><td>MORALES</td><td>02B</td><td>ASP 16 325</td><td>A. Morales et al.</td><td>(COSME Collab.)</td></tr><tr><td>MORALES</td><td>02C</td><td>PL B532 8</td><td>A. Morales et al.</td><td>(IGEX Collab.)</td></tr><tr><td>ABREU</td><td>01</td><td>PL B19 29</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>01B</td><td>PL B19 201</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>BALTAD</td><td>01A</td><td>PL B18 5004</td><td>E. Bätz, P. Gondolo</td><td></td></tr><tr><td>BARATE</td><td>01</td><td>PL B499 67</td><td>R. Barate et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>BARATE</td><td>01B</td><td>PL B19 415</td><td>R. Barate et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>BARGER</td><td>01C</td><td>PL A518 117</td><td>V. Barger, C. Kao</td><td></td></tr><tr><td>BAUDIS</td><td>01</td><td>PR D63 022001</td><td>L. Baudis et al.</td><td>(Heidelberg-Moscow Collab.)</td></tr><tr><td>BERNABEI</td><td>01</td><td>PR D63 197</td><td>R. Bernabei et al.</td><td>(DAMA Collab.)</td></tr><tr><td>BOTTINO</td><td>01</td><td>PR D64 125003</td><td>A. Bottino et al.</td><td></td></tr><tr><td>CORSETTI</td><td>01B</td><td>PR D64 125010</td><td>A. Corsetti, P. Nath</td><td></td></tr><tr><td>ELLIS</td><td>01B</td><td>PL B510 236</td><td>J. Ellis et al.</td><td></td></tr><tr><td>ELLIS</td><td>01C</td><td>PR D63 065016</td><td>J. Ellis, A. Ferstl, K.A. Olive</td><td></td></tr><tr><td>GILZ</td><td>01C</td><td>PL B512 252</td><td>M. Gomez, J. Vergados</td><td></td></tr><tr><td>LAHANAS</td><td>01</td><td>PL B518 94</td><td>A. Lahanas, D.V. Nanopoulos, V. Spanos</td><td></td></tr><tr><td>ABIENDI</td><td>00</td><td>EPJ C12 1</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABIENDI</td><td>00G</td><td>EPJ C14 51</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABIENDI</td><td>00H</td><td>EPJ C14 187</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABIENDI,G</td><td>00D</td><td>EPJ C16 707 (errat.)</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABREU</td><td>00J</td><td>PL B47 129</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABREU</td><td>00Q</td><td>PL B478 65</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>00T</td><td>PL B485 95</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>00U</td><td>PL B487 36</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>00V</td><td>EPJ C3 211</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>00W</td><td>PL B489 38</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>00Z</td><td>EPJ C17 53</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>00D</td><td>PL R84 5699</td><td>R. Abusaidi et al.</td><td>(CDMS Collab.)</td></tr><tr><td>ACCIARRI</td><td>00</td><td>PL R472 420</td><td>M. Acciarri et al.</td><td></td></tr><tr><td>ACCOMANDO</td><td>00</td><td>NP B585 124</td><td>E. Accomando et al.</td><td></td></tr><tr><td>BERNABEI</td><td>00</td><td>PL B480 23</td><td>R. Bernabei et al.</td><td>(DAMA Collab.)</td></tr><tr><td>BERNABEI</td><td>00B</td><td>PL B481 283</td><td>R. Bernabei et al.</td><td>(DAMA Collab.)</td></tr><tr><td>BERNABEI</td><td>00D</td><td>NJP 2 15</td><td>C. Boehm, A. Djoudaji, M. Drees</td><td></td></tr><tr><td>BOEHM</td><td>00B</td><td>PR D62 035012</td><td>J. Ellis et al.</td><td></td></tr><tr><td>ELLIS</td><td>00</td><td>PR D62 075010</td><td>J. Ellis, K. Matchev, F. Wilczek</td><td></td></tr><tr><td>LEP</td><td>00</td><td>PR D62 388</td><td>J. Ellis, K. Matchev, F. Wilczek</td><td></td></tr><tr><td>MORALES</td><td>00</td><td>PL B489 268</td><td>J. Ellis, K. Matchev, F. Wilczek</td><td></td></tr><tr><td>PDG</td><td>00</td><td>PL C15 1</td><td>D. E. Groom et al.</td><td>(PDG Collab.)</td></tr><tr><td>SPOONER</td><td>00</td><td>PL B473 330</td><td>N.J.C. Spooner et al.</td><td>(UK Dark Matter Collab.)</td></tr><tr><td>ACCIARRI</td><td>00</td><td>PL B456 283</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>ACCIARRI</td><td>99R</td><td>PL B470 268</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>ACCIARRI</td><td>99W</td><td>PL B471 280</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>ABRIOSMO</td><td>99</td><td>PR D60 082002</td><td>M. Ambrosio et al.</td><td>(Macro Collab.)</td></tr><tr><td>BAUDIS</td><td>99C</td><td>PR D59 022001</td><td>L. Baudis et al.</td><td>(Heidelberg-Moscow Collab.)</td></tr><tr><td>BELLI</td><td>99C</td><td>PR D53 97</td><td>P. Belli et al.</td><td>(L3 Collab.)</td></tr><tr><td>DOTANI</td><td>99</td><td>PL B461 371</td><td>W. Dotani et al.</td><td></td></tr><tr><td>ABREU</td><td>98P</td><td>PL B444 491</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABREU</td><td>98P</td><td>EPJ C4 207</td><td>M. Acciarri et al.</td><td>(L3 Collab.)</td></tr><tr><td>ACKERSTAFF</td><td>98P</td><td>PL B433 195</td><td>K. Ackerstaff et al.</td><td>(OPAL Collab.)</td></tr><tr><td>BARATE</td><td>98P</td><td>PL B433 176</td><td>R. Barate et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>BARATE</td><td>98P</td><td>EPJ C4 433</td><td>R. Barate et al.</td><td>(DAMA Collab.)</td></tr><tr><td>BERNABEI</td><td>98C</td><td>PL B436 379</td><td>J. Ellis et al.</td><td></td></tr><tr><td>ELLIS</td><td>98B</td><td>PR D58 095002</td><td>J. Ellis, T. Falk, K. Olive</td><td></td></tr><tr><td>ELLIS</td><td>98B</td><td>PL B444 367</td><td>C. Caso et al.</td><td></td></tr><tr><td>BDG</td><td>99</td><td>EPJ C3 1</td><td>H. Baer, M. Brhik</td><td></td></tr><tr><td>BAER</td><td>97</td><td>PR D57 567</td><td>R. Bernabei et al.</td><td></td></tr><tr><td>BERNABEI</td><td>97</td><td>ASP 7 73</td><td>R. Bernabei et al.</td><td></td></tr><tr><td>EDSJO</td><td>97</td><td>PR D56 1879</td><td>J. Edsjo, P. Gondolo</td><td></td></tr><tr><td>ARNOWITT</td><td>96</td><td>PR D54 2374</td><td>R. Arnowitt, P. Nath</td><td></td></tr><tr><td>BAER</td><td>96</td><td>PR D53 597</td><td>H. Baer, M. Brhik</td><td></td></tr><tr><td>BERGSTROM</td><td>96</td><td>ASP 5 263</td><td>L. Bergstrom, P. Gondolo</td><td></td></tr><tr><td>LEWIN</td><td>96</td><td>ASP 6 87</td><td>J.D. Lewin, P.F. Smith</td><td></td></tr><tr><td>BEREZINSKY</td><td>95</td><td>ASP 5 1</td><td>V. Berezinsky et al.</td><td></td></tr><tr><td>FALK</td><td>95</td><td>PL B354 99</td><td>T. Falk, K.A. Olive, M. Srednicki</td><td>(MINN, UCSB)</td></tr><tr><td>LOSECCO</td><td>95</td><td>PL B342 392</td><td>J.M. LoSecco</td><td>(NDAM)</td></tr><tr><td>ADRIANI</td><td>93M</td><td>PRPL 236 1</td><td>O. Adriani et al.</td><td>(L3 Collab.)</td></tr><tr><td>DREES</td><td>93</td><td>PL D47 397</td><td>M. Drees, M.M. Nojiri</td><td></td></tr><tr><td>DREES</td><td>93B</td><td>PR D48 3483</td><td>M. Drees, M.M. Nojiri</td><td>(DESY, SLAC)</td></tr><tr><td>FALK</td><td>93</td><td>PL B318 354</td><td>T. Falk et al.</td><td>(UCB, UCSB, MINN)</td></tr><tr><td>KELLEY</td><td>93</td><td>PR D47 2461</td><td>S. Kelley et al.</td><td>(TAMU, ALAH)</td></tr><tr><td>MIZUTA</td><td>93</td><td>PL B298 120</td><td>S. Mizuta, M. Yamaguchi</td><td>(TOHO)</td></tr><tr><td>MURB</td><td>93</td><td>PL D50 5055</td><td>M. Mori et al.</td><td>(KEK, NIIG, TOKY, TOKA)</td></tr><tr><td>BOTTINO</td><td>92</td><td>MPL A7 733</td><td>A. Böttino et al.</td><td>(ZARA, ZORA)</td></tr><tr><td>DECAMP</td><td>92</td><td>PL B265 57</td><td>A. Böttino et al.</td><td>(TORI, INFN)</td></tr><tr><td>LOPEZ</td><td>92</td><td>NP B370 445</td><td>D. Decamp et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>MONDALE</td><td>92</td><td>PL B283 30</td><td>J. McDonald, K.A. Olive, M. Srednicki</td><td>(TAMU)</td></tr><tr><td>ABREU</td><td>92</td><td>NP B367 511</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ALEXANDER</td><td>91F</td><td>PZY C56 175</td><td>G. Alexander et al.</td><td>(OPAL Collab.)</td></tr><tr><td>BOTTINO</td><td>91F</td><td>PL B25 57</td><td>A. Böttino et al.</td><td>(TORI, INFN)</td></tr><tr><td>GELMINI</td><td>91</td><td>NP B351 623</td><td>G. Gellini et al.</td><td></td></tr><tr><td>GRIEST</td><td>91</td><td>PR D43 319</td><td>K. Griest, D. Seckel</td><td></td></tr><tr><td>KAMIONKOW...</td><td>91</td><td>PR D44 3021</td><td>M. Kamionkowski</td><td>(CHIC, FNAL)</td></tr><tr><td>MORI</td><td>91B</td><td>PL B270 89</td><td>M. Mori et al.</td><td>(Kamiokande Collab.)</td></tr><tr><td>NOJRI</td><td>91</td><td>PL B261 76</td><td>M.M. Nojiri</td><td></td></tr><tr><td>Olive</td><td>91</td><td>NP B355 208</td><td>K. Olive, M. Srednicki</td><td>(MINN, UCSB)</td></tr><tr><td>ROSKOWSKI</td><td>91</td><td>NP B352 59</td><td>L. Roszkowski</td><td>(CERN)</td></tr><tr><td>GRIEST</td><td>90</td><td>PR D41 3565</td><td>R. Barbieri, M. Frigeni, G. Giudice</td><td>(UCB+)</td></tr><tr><td>BARBIERI</td><td>89C</td><td>NP B313 725</td><td>K. A. Olive, M. Srednicki</td><td></td></tr><tr><td>Olive</td><td>79</td><td>NP B230 78</td><td>K. A. Olive, M. Srednicki</td><td></td></tr><tr><td>ELLIS</td><td>88D</td><td>NP B307 883</td><td>J. Ellis, R. Flores</td><td></td></tr></tbody></table>
<table><tr><td>GRIEST</td><td>88B</td><td>PR D38 2357</td><td>K. Griest</td><td></td></tr><tr><td>OLIVE</td><td>88</td><td>PL B205 553</td><td>K.A. Olive, M. Srednicki</td><td>(MINN, UCSB)</td></tr><tr><td>SREDNICKI</td><td>88</td><td>NP B310 693</td><td>M. Srednicki, R. Watkins, K.A. Olive</td><td>(MINN, UCSB)</td></tr><tr><td>ELLIS</td><td>84</td><td>NP B238 453</td><td>J. Ellis et al.</td><td>(CERN)</td></tr><tr><td>GOLDBERG</td><td>83</td><td>PRL 50 1419</td><td>H. Goldberg</td><td>(NEAS)</td></tr><tr><td>KRAUSS</td><td>83</td><td>NP B227 556</td><td>L.M. Krauss</td><td>(HARV)</td></tr><tr><td>VYSOTSKII</td><td>83</td><td>SJNP 37 948</td><td>M.L. Vysotsky</td><td>(ITEP)</td></tr></table>

Translated from YAF 37 1597.

Technicolor

See the related review(s):

Dynamical Electroweak Symmetry Breaking: Implications of the H⁰

The latest unpublished results are described in "Dynamical Electroweak Symmetry Breaking" review.

### MASS LIMITS for Resonances in Models of Dynamical Electroweak Symmetry Breaking

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;3900</td><td>95</td><td>1 AAD</td><td>20AMATLS</td><td>top-color Z'</td></tr><tr><td></td><td></td><td>2 AAD</td><td>20W ATLS</td><td>ρ<sub>T</sub> → Wπ<sub>T</sub> → ℓνq<span style="text-decoration: overline">q</span></td></tr><tr><td></td><td></td><td>3 AAD</td><td>16W ATLS</td><td>color octet vector resonance</td></tr><tr><td>&gt;2400</td><td>95</td><td>4 KHACHATRY..16E</td><td>CMS</td><td>top-color Z'</td></tr><tr><td></td><td></td><td>5 AAD</td><td>15AB ATLS</td><td>h → π<sub>V</sub>π<sub>V</sub></td></tr><tr><td></td><td></td><td>6 AAD</td><td>15AO ATLS</td><td>top-color Z'</td></tr><tr><td></td><td></td><td>7 AAD</td><td>15BB ATLS</td><td>pp → ρ<sub>T</sub>/a<sub>1</sub>T → Wh or Zh</td></tr><tr><td></td><td></td><td>8 AAD</td><td>15Q ATLS</td><td>h → π<sub>V</sub>π<sub>V</sub></td></tr><tr><td></td><td></td><td>9 AAIJ</td><td>15AN LHCB</td><td>h → π<sub>V</sub>π<sub>V</sub></td></tr><tr><td>&gt;1140</td><td>95</td><td>10 KHACHATRY..15C</td><td>CMS</td><td>ρ<sub>T</sub> → WZ</td></tr><tr><td></td><td></td><td>11 KHACHATRY..15W</td><td>CMS</td><td>H → π<sub>V</sub>π<sub>V</sub></td></tr><tr><td></td><td></td><td>12 AAD</td><td>14AT ATLS</td><td>pp → ω<sub>T</sub> → Zγ</td></tr><tr><td>none 200-700, 750-890</td><td>95</td><td>12 AAD</td><td>14AT ATLS</td><td>pp → a<sub>T</sub> → Wγ</td></tr><tr><td>none 275-960</td><td>95</td><td>13 AAD</td><td>14V ATLS</td><td>color singlet techni-vector</td></tr><tr><td></td><td></td><td>14 AAD</td><td>13AN ATLS</td><td>pp → a<sub>T</sub> → Wγ</td></tr><tr><td></td><td></td><td>15 AAD</td><td>13AN ATLS</td><td>pp → ω<sub>T</sub> → Zγ</td></tr><tr><td>none 500-1740</td><td>95</td><td>16 AAD</td><td>13AQ ATLS</td><td>top-color Z'</td></tr><tr><td>&gt;1300</td><td>95</td><td>17 CHATRCHYAN 13AP</td><td>CMS</td><td>top-color Z'</td></tr><tr><td>&gt;2100</td><td>95</td><td>16 CHATRCHYAN 13BM</td><td>CMS</td><td>top-color Z'</td></tr><tr><td></td><td></td><td>18 BAAK</td><td>12 RVUE</td><td>QCD-like technicolor</td></tr><tr><td>none 167-687</td><td>95</td><td>19 CHATRCHYAN 12AF</td><td>CMS</td><td>ρ<sub>T</sub> → WZ</td></tr><tr><td></td><td></td><td>16 AALTONEN</td><td>11AD CDF</td><td>top-color Z'</td></tr><tr><td></td><td></td><td>16 AALTONEN</td><td>11AE CDF</td><td>top-color Z'</td></tr><tr><td></td><td></td><td>20 CHIVUKULA</td><td>11 RVUE</td><td>top-Higgs</td></tr><tr><td></td><td></td><td>21 CHIVUKULA</td><td>11A RVUE</td><td>techni-π</td></tr><tr><td></td><td></td><td>22 AALTONEN</td><td>10I CDF</td><td>ρ<span style="text-decoration: overline">b</span> → ρ<sub>T</sub>/ω<sub>T</sub> → Wπ<sub>T</sub></td></tr><tr><td>none 208-408</td><td>95</td><td>23 ABAZOV</td><td>10A D0</td><td>ρ<sub>T</sub> → WZ</td></tr><tr><td></td><td></td><td>24 ABAZOV</td><td>07I D0</td><td>ρ<span style="text-decoration: overline">b</span> → ρ<sub>T</sub>/ω<sub>T</sub> → Wπ<sub>T</sub></td></tr><tr><td></td><td></td><td>25 ABULENCIA</td><td>05A CDF</td><td>ρ<sub>T</sub> → e<sup>+</sup>e<sup>-</sup>, μ<sup>+</sup>μ<sup>-</sup></td></tr><tr><td></td><td></td><td>26 CHEKANOV</td><td>02B ZEUS</td><td>color octet techni-π</td></tr><tr><td></td><td></td><td>27 ABAZOV</td><td>01B D0</td><td>ρ<sub>T</sub> → e<sup>+</sup>e<sup>-</sup></td></tr><tr><td>none 90-206.7</td><td>95</td><td>28 ABDALLAH</td><td>01 DLPH</td><td>e<sup>+</sup>e<sup>-</sup> → ρ<sub>T</sub></td></tr><tr><td></td><td></td><td>29 AFFOLDER</td><td>00F CDF</td><td>color-singlet techni-ρ<sub>T</sub>, ρ<sub>T</sub> → Wπ<sub>T</sub>, 2π<sub>T</sub></td></tr><tr><td></td><td></td><td>30 AFFOLDER</td><td>00K CDF</td><td>color-octet techni-ρ<sub>T</sub>, ρ<sub>T</sub> → 2π<sub>LQ</sub></td></tr><tr><td>none 350-440</td><td>95</td><td>31 ABE</td><td>99F CDF</td><td>color-octet techni-ρ<sub>T</sub>, ρ<sub>T</sub> → <span style="text-decoration: overline">b</span>b</td></tr><tr><td></td><td></td><td>32 ABE</td><td>99N CDF</td><td>techni-ω, ω<sub>T</sub> → γ<span style="text-decoration: overline">b</span>b</td></tr><tr><td>none 260-480</td><td>95</td><td>33 ABE</td><td>97G CDF</td><td>color-octet techni-ρ<sub>T</sub>, ρ<sub>T</sub> → 2jets</td></tr></tbody></table>

### REFERENCES FOR Technicolor

<table><tr><td>AAD</td><td>20AM JHEP 2010 061</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20W JHEP 2006 151</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16W PL B758 249</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>KHACHATRY..16E PR D91 02001</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>15AB PR D92 012010</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15AO JHEP 1508 148</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15BB EPJ C75 263</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15Q PL B743 15</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15AN PR D75 152</td><td>R. Aaij et al.</td><td>(LHCb Collab.)</td></tr><tr><td>AAD</td><td>KHACHATRY..15C PR B740 83</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>KHACHATRY..15W PR D91 052012</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>14AT PL B738 428</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>14V PR D90 052005</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>13AN PR D87 112003</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>Also PR D91 119901 (errat.)</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>13AQ PR D88 012004</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>CHATRCHYAN</td><td>13AP PR D87 072002</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRCHYAN</td><td>13BM PRL 111 211804</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>Also</td><td>PRL 112 119903 (errat.)</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>BAAK</td><td>12 EPI C72 2003</td><td>M. Baak et al.</td><td>(Gritter Group)</td></tr><tr><td>CHATRCHYAN</td><td>12AF PR 109 141801</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AALTONEN</td><td>11AD PR D84 072003</td><td>T. Aaltonen et al.</td><td>(CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>11AE PR D84 072004</td><td>T. Aaltonen et al.</td><td>(CDF Collab.)</td></tr><tr><td>CHIVUKULA</td><td>11A PR D84 095022</td><td>R.S. Chivukula et al.</td><td>(CDF Collab.)</td></tr><tr><td>CHIVUKULA</td><td>11I PR D84 115025</td><td>R. S. Chivukula et al.</td><td>(CDF Collab.)</td></tr><tr><td>AALTONEN</td><td>10I PRL 104 111802</td><td>T. Aaltonen et al.</td><td>(CDF Collab.)</td></tr></table>

<footnote n="1">¹AAD 20AM search for a top-color Z' decaying to t<span style="text-decoration: overline">t</span> in pp collisions at $\sqrt{s} = 13$ TeV. The quoted limit is for $\Gamma Z'/M_{Z'} = 0.01$. The limit becomes $M_{Z'} > 4700$ GeV for $\Gamma Z'/M_{Z'} = 0.03$.</footnote>

<footnote n="2">²AAD 20W search for techni-ρ decaying to π<sub>T</sub> W in pp collisions at $\sqrt{s} = 13$ TeV. See their Fig. 5a for limits on σ·B.</footnote>

<footnote n="3">³AAD 16W search for color octet vector resonance decaying to b<span style="text-decoration: overline">b</span> in pp collisions at $\sqrt{s} = 8$ TeV. The vector or quark B is assumed to decay to b<span style="text-decoration: overline">H</span>. See their Fig.3 and Fig.4 for limits on σ·B.</footnote>

<footnote n="4">⁴KHACHATRYAN 16E search for top-color Z' decaying to t<span style="text-decoration: overline">t</span>. The quoted limit is for $\Gamma Z'/m_{Z'} = 0.012$. Also exclude $m_{Z'} < 2.9$ TeV for wider topcolor Z' with $\Gamma Z'/m_{Z'} = 0.1$.</footnote>

<footnote n="5">⁵AAD 15AB search for long-lived hidden valley π<sub>V</sub> particles which are produced in pairs by the decay of a scalar boson. π<sub>V</sub> is assumed to decay into dijets. See their Fig. 10 for the limit on σ·B.</footnote>

<footnote n="6">⁶AAD 15AO search for top-color Z' decaying to t<span style="text-decoration: overline">t</span>. The quoted limit is for $\Gamma Z'/m_{Z'} = 0.012$.</footnote>

<footnote n="7">⁷AAD 15BB search for minimal walking technicolor (MWT) isotriplet vector and axial-vector resonances decaying to W or Zh. See their Fig. 3 for the exclusion limit in the MWT parameter space.</footnote>

<footnote n="8">⁸AAD 15q search for long-lived hidden valley π<sub>V</sub> particles which are produced in pairs by the decay of scalar boson. π<sub>V</sub> is assumed to decay into dijets. See their Fig. 5 and Fig. 6 for the limit on σ·B.</footnote>

<footnote n="9">⁹AAIJ 15AN search for long-lived hidden valley π<sub>V</sub> particles which are produced in pairs by the decay of scalar boson with a mass of 120GeV. π<sub>V</sub> is assumed to decay into dijets. See their Fig. 4 for the limit on σ·B.</footnote>

<footnote n="10">¹⁰KHACHATRYAN 15C search for a vector techni-resonance decaying to WZ. The limit assumes $M_{π_T} = (3/4) M_{ρ_T} - 25$ GeV. See their Fig.3 for the limit in $M_{π_T} - M_{ρ_T}$ plane of the low scale technicolor model.</footnote>

<footnote n="11">¹¹KHACHATRYAN 15W search for long-lived hidden valley π<sub>V</sub> particles which are produced in pairs in the decay of heavy higgs boson H. π<sub>V</sub> is assumed to decay into $ℓ^+ℓ^-$. See their Fig. 7 and Fig. 8 for the limits on σB.</footnote>

<footnote n="12">¹²AAD 14AT search for techni-ω and techni-a resonances decaying to Vγ with V = W(→ $ℓν$) or Z(→ $ℓ^+ℓ^-$).</footnote>

<footnote n="13">¹³AAD 14V search for vector techni-resonances decaying into electron or muon pairs in pp collisions at $\sqrt{s} = 8$ TeV. See their table IX for exclusion limits with various assumptions.</footnote>

<footnote n="14">¹⁴AAD 13AN search for vector techni-resonance a<sub>T</sub> decaying into Wγ.</footnote>

<footnote n="15">¹⁵AAD 13AN search for vector techni-resonance ω<sub>T</sub> decaying into Zγ.</footnote>

<footnote n="16">¹⁶Search for top-color Z' decaying to t<span style="text-decoration: overline">t</span>. The quoted limit is for $\Gamma Z'/m_{Z'} = 0.012$.</footnote>

<footnote n="17">¹⁷CHATRCHYAN 13AP search for top-color leptophobic Z' decaying to t<span style="text-decoration: overline">t</span>. The quoted limit is for $\Gamma Z'/m_{Z'} = 0.012$.</footnote>

<footnote n="18">¹⁸BAAK 12 give electroweak oblique parameter constraints on the QCD-like technicolor models. See their Fig. 28.</footnote>

<footnote n="19">¹⁹CHATRCHYAN 12AF search for a vector techni-resonance decaying to WZ. The limit assumes $M_{π_T} = (3/4) M_{ρ_T} - 25$ GeV. See their Fig. 3 for the limit in $M_{π_T} - M_{ρ_T}$ plane of the low scale technicolor model.</footnote>

<footnote n="20">²⁰Using the LHC limit on the Higgs boson production cross section, CHIVUKULA 11 obtain a limit on the top-Higgs mass > 300 GeV at 95% CL assuming 150 GeV top-pion mass.</footnote>

<footnote n="21">²¹Using the LHC limit on the Higgs boson production cross section, CHIVUKULA 11A obtain a limit on the technipion mass ruling out the region 110 GeV < m<sub>P</sub> < 2m<sub>T</sub>. Existence of color techni-fermions, top-color mechanism, and N<sub>TC</sub> ≥ 3 are assumed.</footnote>

<footnote n="22">²²AALTONEN 10I search for the vector techni-resonances (ρ<sub>T</sub>, ω<sub>T</sub>) decaying into Wπ<sub>T</sub> with W → $ℓν$ and π<sub>T</sub> → b<span style="text-decoration: overline">b</span>, b<span style="text-decoration: overline">c</span>, or b<span style="text-decoration: overline">W</span>. See their Fig. 3 for the exclusion plot in $M_{π_T} - M_{ρ_T}$ plane.</footnote>

<footnote n="23">²³ABAZOV 10A search for a vector techni-resonance (ρ<sub>T</sub>, ω<sub>T</sub>) decaying into Wπ<sub>T</sub> with W → eν and π<sub>T</sub> → b<span style="text-decoration: overline">b</span> or b<span style="text-decoration: overline">c</span>. See their Fig. 2 for the exclusion plot in $M_{π_T} - M_{ρ_T}$ plane.</footnote>

<footnote n="24">²⁴ABAZOV 07I search for the vector techni-resonances (ρ<sub>T</sub>, ω<sub>T</sub>) decaying into Wπ<sub>T</sub> with W → eν and π<sub>T</sub> → b<span style="text-decoration: overline">b</span> or b<span style="text-decoration: overline">c</span>. See their Fig. 2 for the exclusion plot in $M_{π_T} - M_{ρ_T}$ plane.</footnote>

<footnote n="25">²⁵ABULENCIA 05A search for resonances decaying to electron or muon pairs in p<span style="text-decoration: overline">p</span> collisions. at $\sqrt{s} = 1.96$ TeV. The limit assumes Technicolor-scale mass parameters M<sub>V</sub> = M<sub>A</sub> = 500 GeV.</footnote>

<footnote n="26">²⁶CHEKANOV 02B search for color octet techni-π P decaying into dijets in e<sub>P</sub> collisions. See their Fig. 5 for the limit on σ(e<sub>P</sub> → e<sub>X</sub>)·B(P → 2j).</footnote>

<footnote n="27">²⁷ABAZOV 01B search for vector techni-resonances (ρ<sub>T</sub>, ω<sub>T</sub>) decaying to e<sup>+</sup>e<sup>-</sup>. The limit assumes $M_{ρ_T} = M_{ω_T} < M_{π_T} + M_W$.</footnote>

<footnote n="28">²⁸The limit is independent of the π<sub>T</sub> mass. See their Fig. 9 and Fig. 10 for the exclusion plot in the $M_{ρ_T} - M_{π_T}$ plane. ABDALLAH 01 limit on the techni-pion mass is $M_{π_T} > 79.8$ GeV for N<sub>D</sub>=2, assuming its point-like coupling to gauge bosons.</footnote>

<footnote n="29">²⁹AFFOLDER 00F search for ρ<sub>T</sub> decaying into Wπ<sub>T</sub> or π<sub>T</sub>π<sub>T</sub> with W → $ℓν$ and π<sub>T</sub> → b<span style="text-decoration: overline">b</span>, b<span style="text-decoration: overline">c</span>. See Fig. 1 in the above Note on "Dynamical Electroweak Symmetry Breaking" for the exclusion plot in the $M_{ρ_T} - M_{π_T}$ plane.</footnote>

<footnote n="30">³⁰AFFOLDER 00K search for the ρ<sub>T</sub>8 decaying into π<sub>LQ</sub>π<sub>LQ</sub> with π<sub>LQ</sub> → b<sup>+</sup>. For π<sub>LQ</sub> → c<sup>+</sup>, the limit is $M_{ρT8} > 510$ GeV. See their Fig. 2 and Fig. 3 for the exclusion plot in the $M_{ρT8} - M_{πLQ}$ plane.</footnote>

<footnote n="31">³¹ABE 99F search for a new particle X decaying into b<span style="text-decoration: overline">b</span> in p<span style="text-decoration: overline">p</span> collisions at $E_{cm} = 1.8$ TeV. See Fig. 7 in the above Note on "Dynamical Electroweak Symmetry Breaking" for the upper limit on σ(p<span style="text-decoration: overline">p</span> → X)×B(X → b<span style="text-decoration: overline">b</span>). ABE 99f also exclude top gluons of width Γ=0.3M in the mass interval 280 < M < 670 GeV, of width Γ=0.5M in the mass interval 340 < M < 640 GeV, and of width Γ=0.7M in the mass interval 375 < M < 560 GeV.</footnote>

<footnote n="32">³²ABE 99N search for the techni-ω decaying into γπ<sub>T</sub>. The technipion is assumed to decay π<sub>T</sub> → b<span style="text-decoration: overline">b</span>. See Fig. 2 in the above Note on "Dynamical Electroweak Symmetry Breaking" for the exclusion plot in the $M_{π_T} - M_{π_T}$ plane.</footnote>

<footnote n="33">³³ABE 97G search for a new particle X decaying into dijets in p<span style="text-decoration: overline">p</span> collisions at $E_{cm} = 1.8$ TeV. See Fig. 5 in the above Note on "Dynamical Electroweak Symmetry Breaking" for the upper limit on σ(p<span style="text-decoration: overline">p</span> → X)×B(X → 2j).</footnote>
<table><tr><td>ABAZOV</td><td>10A</td><td>PRL 104 061801</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ABAZOV</td><td>07I</td><td>PRL 98 221801</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ABULENCIA</td><td>05A</td><td>PRL 95 252001</td><td>A. Abulencia et al.</td><td>(CDF Collab.)</td></tr><tr><td>CHEKANOV</td><td>02B</td><td>PL B531 9</td><td>S. Chekanov et al.</td><td>(ZEUS Collab.)</td></tr><tr><td>ABAZOV</td><td>01B</td><td>PRL 87 061802</td><td>V.M. Abazov et al.</td><td>(D0 Collab.)</td></tr><tr><td>ABDALLAH</td><td>01</td><td>EPJ C22 17</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>AFFOLDER</td><td>00F</td><td>PRL 84 11110</td><td>T. Affolder et al.</td><td>(CDF Collab.)</td></tr><tr><td>AFFOLDER</td><td>00K</td><td>PRL 85 2056</td><td>T. Affolder et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABE</td><td>99F</td><td>PRL 82 2038</td><td>F. Abe et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABE</td><td>99N</td><td>PRL 83 3124</td><td>F. Abe et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABE</td><td>97G</td><td>PR D55 5263</td><td>F. Abe et al.</td><td>(CDF Collab.)</td></tr></table>

## Quark and Lepton Compositeness, Searches for

The latest unpublished results are described in the “Quark and Lepton Compositeness” review.

See the related review(s):

Searches for Quark and Lepton Compositeness

### CONTENTS:

* Scale Limits for Contact Interactions: $\Lambda(eeee)$

* Scale Limits for Contact Interactions: $\Lambda(ee\mu\mu)$

* Scale Limits for Contact Interactions: $\Lambda(ee\tau\tau)$

* Scale Limits for Contact Interactions: $\Lambda(\ell\ell\ell\ell)$

* Scale Limits for Contact Interactions: $\Lambda(eeqq)$

* Scale Limits for Contact Interactions: $\Lambda(\mu\mu\mu\mu)$

* Scale Limits for Contact Interactions: $\Lambda(\ell\nu\ell\nu)$

* Scale Limits for Contact Interactions: $\Lambda(e\nu\nu\nu)$

* Scale Limits for Contact Interactions: $\Lambda(qqqq)$

* Scale Limits for Contact Interactions: $\Lambda(\nu\nu\nu\nu)$

* Mass Limits for Excited $e$ ($e^*$)

- Limits for Excited $e$ ($e^*$) from Pair Production

- Limits for Excited $e$ ($e^*$) from Single Production

- Limits for Excited $e$ ($e^*$) from $e^+e^- \to \gamma\gamma$

- Indirect Limits for Excited $e$ ($e^*$)

* Mass Limits for Excited $\mu$ ($\mu^*$)

- Limits for Excited $\mu$ ($\mu^*$) from Pair Production

- Limits for Excited $\mu$ ($\mu^*$) from Single Production

- Indirect Limits for Excited $\mu$ ($\mu^*$)

* Mass Limits for Excited $\tau$ ($\tau^*$)

- Limits for Excited $\tau$ ($\tau^*$) from Pair Production

- Limits for Excited $\tau$ ($\tau^*$) from Single Production

* Mass Limits for Excited Neutrino ($\nu^*$)

- Limits for Excited $\nu$ ($\nu^*$) from Pair Production

- Limits for Excited $\nu$ ($\nu^*$) from Single Production

* Mass Limits for Excited $q$ ($q^*$)

- Limits for Excited $q$ ($q^*$) from Pair Production

- Limits for Excited $q$ ($q^*$) from Single Production

* Mass Limits for Color Sextet Quarks ($q_8$)

* Mass Limits for Color Octet Charged Leptons ($\ell_8$)

* Mass Limits for Color Octet Neutrinos ($\nu_8$)

* Mass Limits for $W_8$ (Color Octet W Boson)

### SCALE LIMITS for Contact Interactions: $\Lambda(eeee)$

Limits are for $\Lambda_{LL}^{\pm}$ only. For other cases, see each reference.

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>-</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;8.3</td><td>&gt;10.3</td><td>95</td><td>1 BOURILKOV</td><td>01</td><td>RVUE E<sub>cm</sub> = 192-208 GeV</td></tr></tbody></table>

1 A combined analysis of the data from ALEPH, DELPHI, L3, and OPAL.

2 SCHAEL 07A limits are from $R_c$, $Q_{FB}^{depl}$, and hadronic cross section measurements.

3 ABIENDI 04G limits are from $e^+e^- \to e^+e^-$ cross section at $\sqrt{s} = 130-207$ GeV.

### SCALE LIMITS for Contact Interactions: $\Lambda(ee\mu\mu)$

Limits are for $\Lambda_{LL}^{\pm}$ only. For other cases, see each reference.

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>-</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>>6.6</td><td>>9.5</td><td>95</td><td>1 SCHAEL</td><td>07A</td><td>ALEP E<sub>cm</sub> = 189-209 GeV</td></tr><tr><td>> 8.5</td><td>>3.8</td><td>95</td><td>ABIENDI</td><td>00P</td><td>L3 E<sub>cm</sub> = 130-189 GeV</td></tr></tbody></table>

1 SCHAEL 07A limits are from $R_c$, $Q_{FB}^{depl}$, and hadronic cross section measurements.

2 ABIENDI 04G limits are from $e^+e^- \to \mu\mu$ cross section at $\sqrt{s} = 130-207$ GeV.

### SCALE LIMITS for Contact Interactions: $\Lambda(ee\tau\tau)$

Limits are for $\Lambda_{LL}^{\pm}$ only. For other cases, see each reference.

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>-</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>>7.9</td><td>>5.8</td><td>95</td><td>1 SCHAEL</td><td>07A</td><td>ALEP E<sub>cm</sub> = 189-209 GeV</td></tr><tr><td>>7.9</td><td>>4.6</td><td>95</td><td>ABDALLAH</td><td>06C</td><td>DLPH E<sub>cm</sub> = 130-207 GeV</td></tr><tr><td>>4.9</td><td>>7.2</td><td>95</td><td>2 ABIENDI</td><td>04G</td><td>OPAL E<sub>cm</sub> = 130-207 GeV</td></tr></tbody></table>

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

<table><tr><td>>5.4</td><td>>4.7</td><td>95</td><td>ACCIARRI</td><td>00P</td><td>L3 E<sub>cm</sub> = 130-189 GeV</td></tr></table>

1 SCHAEL 07A limits are from $R_c$, $Q_{FB}^{depl}$, and hadronic cross section measurements.

2 ABIENDI 04G limits are from $e^+e^- \to \tau\tau$ cross section at $\sqrt{s} = 130-207$ GeV.

### SCALE LIMITS for Contact Interactions: $\Lambda(\ell\ell\ell\ell)$

Lepton universality assumed. Limits are for $\Lambda_{LL}^{\pm}$ only. For other cases, see each reference.

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>-</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>>7.9</td><td>>10.3</td><td>95</td><td>1 SCHAEL</td><td>07A</td><td>ALEP E<sub>cm</sub> = 189-209 GeV</td></tr><tr><td>>9.1</td><td>>8.2</td><td>95</td><td>ABDALLAH</td><td>06C</td><td>DLPH E<sub>cm</sub> = 130-207 GeV</td></tr></tbody></table>

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

<table><tr><td>>7.7</td><td>>9.5</td><td>95</td><td>2 ABIENDI</td><td>04G</td><td>OPAL E<sub>cm</sub> = 130-207 GeV</td></tr><tr><td>>9.0</td><td>>5.2</td><td>95</td><td>3 BABICH</td><td>03</td><td>RVUE E<sub>cm</sub> = 130-189 GeV</td></tr></table>

1 SCHAEL 07A limits are from $R_c$, $Q_{FB}^{depl}$, and hadronic cross section measurements.

2 ABIENDI 04G limits are from $e^+e^- \to \ell^+\ell^-$ cross section at $\sqrt{s} = 130-207$ GeV.

3 BABICH 03 obtain a bound $-0.175 \text{ TeV}^{-2} < 1/\Lambda_{LL}^2 < 0.095 \text{ TeV}^{-2}$ (95%CL) in a model independent analysis allowing all of $\Lambda_{LL}$, $\Lambda_{LR}$, $\Lambda_{RL}$, $\Lambda_{RR}$ to coexist.

### SCALE LIMITS for Contact Interactions: $\Lambda(eeqq)$

Limits are for $\Lambda_{LL}^{\pm}$ only. For other cases, see each reference.

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>-</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>>24</td><td>>37</td><td>95</td><td>1 AABOUD</td><td>17AT</td><td>ATLS (eeqq)</td></tr><tr><td>> 8.4</td><td>>10.2</td><td>95</td><td>2 ABDALLAH</td><td>09</td><td>DLPH (eebb)</td></tr><tr><td>> 9.4</td><td>>5.6</td><td>95</td><td>3 SCHAEL</td><td>07A</td><td>ALEP (eecc)</td></tr><tr><td>> 9.4</td><td>>4.9</td><td>95</td><td>2 SCHAEL</td><td>07A</td><td>ALEP (eebb)</td></tr><tr><td>>23.3</td><td>>12.5</td><td>95</td><td>4 CHEUNG</td><td>01B</td><td>RVUE (eeuu)</td></tr><tr><td>>11.1</td><td>>26.4</td><td>95</td><td>4 CHEUNG</td><td>01B</td><td>RVUE (eedd)</td></tr></tbody></table>

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

<table><tr><td>> 7.1</td><td>>7.1</td><td>95</td><td>5 AAD</td><td>21AU</td><td>ATLS (eebs)</td></tr><tr><td>>23.5</td><td>>26.1</td><td>95</td><td>6 AAD</td><td>21Q</td><td>ATLS (eeqq)</td></tr><tr><td>>19.5</td><td>>24.0</td><td>95</td><td>7 SIRUNYAN</td><td>21N</td><td>CMS (eeqq)</td></tr><tr><td>>23.5</td><td>>26.1</td><td>95</td><td>8 AAD</td><td>20AP</td><td>ATLS (eeqq)</td></tr><tr><td>> 4.5</td><td>>12.8</td><td>95</td><td>9 ABRAMOWICZ</td><td>19</td><td>ZEUS (eeqq)</td></tr><tr><td>>16.8</td><td>>23.9</td><td>95</td><td>10 SIRUNYAN</td><td>19AC</td><td>CMS (eeqq)</td></tr><tr><td>>15.5</td><td>>19.5</td><td>95</td><td>11 AABOUD</td><td>16U</td><td>ATLS (eeqq)</td></tr><tr><td>>13.5</td><td>>18.3</td><td>95</td><td>12 KHACHATRY</td><td>15AE</td><td>CMS (eeqq)</td></tr><tr><td>>16.4</td><td>>20.7</td><td>95</td><td>13 AAD</td><td>14BE</td><td>ATLS (eeqq)</td></tr><tr><td>> 9.5</td><td>>12.1</td><td>95</td><td>14 AAD</td><td>13E</td><td>ATLS (eeqq)</td></tr><tr><td>>10.1</td><td>>9.4</td><td>95</td><td>15 AAD</td><td>12AB</td><td>ATLS (eeqq)</td></tr><tr><td>> 4.2</td><td>>4.0</td><td>95</td><td>16 AARON</td><td>11C</td><td>H1 (eeqq)</td></tr><tr><td>> 3.8</td><td>>3.8</td><td>95</td><td>17 ABDALLAH</td><td>11</td><td>DLPH (eetc)</td></tr><tr><td>>12.9</td><td>>7.2</td><td>95</td><td>18 SCHAEL</td><td>07A</td><td>ALEP (eeqq)</td></tr><tr><td>> 3.7</td><td>>5.9</td><td>95</td><td>19 ABIULENCIA</td><td>06L</td><td>CDF (eeqq)</td></tr></tbody></table>

1 AABOUD 17AT limits are from $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit uses a uniform positive prior in $1/\Lambda^2$.

2 ABDALLAH 09 and SCHAEL 07A limits are from $R_b$, $A_b^{FB}$.

3 SCHAEL 07A limits are from $R_c$, $Q_{FB}^{depl}$, and hadronic cross section measurements.

4 CHEUNG 01B is an update of BARGER 98E.

5 AAD 21AU search for new phenomena in final states with $e^+e^-$ and one or no b-tagged jets in $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limits assume $g_s^2 = 4 \pi$.

6 AAD 21Q limits are from $pp$ collisions at $\sqrt{s} = 13$ TeV. A frequentist statistical framework is used to remove the prior dependence.

7 SIRUNYAN 21N limits are from $e^+e^-$ mass distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV.

8 AAD 20AP limits are from $e^+e^-$ mass distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV.

9 ABRAMOWICZ 19 limits are from $Q^2$ spectrum measurements of $e^\pm p \to e^\pm X$.

10 SIRUNYAN 19AC limits are from $e^+e^-$ mass distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV.

11 AABOUD 16U limits are from $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit uses a uniform positive prior in $1/\Lambda^2$.

12 KHACHATRYAN 15AE limit is from $e^+e^-$ mass distribution in $pp$ collisions at $E_{cm} = 8$ TeV.

13 AAD 14BE limits are from $pp$ collisions at $\sqrt{s} = 8$ TeV. The quoted limit uses a uniform positive prior in $1/\Lambda^2$.

14 AAD 13E limits are from $e^+e^-$ mass distribution in $pp$ collisions at $E_{cm} = 7$ TeV.

15 AAD 12AB limits are from $e^+e^-$ mass distribution in $pp$ collisions at $E_{cm} = 7$ TeV.

16 AARON 11C limits are from $Q^2$ spectrum measurements of $e^\pm p \to e^\pm X$.

17 ABDALLAH 11 limit is from $e^+e^- \to t\bar{c}$ cross section. $\Lambda_{LL} = \Lambda_{LR} = \Lambda_{RL} = \Lambda_{RR}$ is assumed.

18 SCHAEL 07A limit assumes quark flavor universality of the contact interactions.

19 ABIULENCIA 06L limits are from $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV.
SCALE LIMITS for Contact Interactions: $\Lambda(\mu\mu qq)$

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;23.3</strong></td><td><strong>&gt;40.0</strong></td><td>95</td><td>1 SIRUNYAN</td><td>21N</td><td>CMS (μμqq)</td></tr></tbody></table>

1 SIRUNYAN 21N limits are from $\mu^+\mu^-$ mass distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV.

2 AAD 21AU search for new phenomena in final states with $\mu^+\mu^-$ and one or no b-tagged jets in $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limits assume $g_*^2 = 4$ π.

3 AAD 21Q limits are from $pp$ collisions at $\sqrt{s} = 13$ TeV. A frequentist statistical framework is used to remove the prior dependence.

4 AAD 20AP limits are from $\mu^+\mu^-$ mass distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV.

5 SIRUNYAN 19AC limits are from $\mu^+\mu^-$ mass distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV.

6 AABOUD 17AT limits are from $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit uses a uniform positive prior in $1/\Lambda^2$.

7 AABOUD 16U limits are from $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit uses a uniform positive prior in $1/\Lambda^2$.

8 KHACHATRYAN 15AE limit is from $\mu^+\mu^-$ mass distribution in $pp$ collisions at $E_{cm} = 8$ TeV.

9 AAD 14BE limits are from $pp$ collisions at $\sqrt{s} = 8$ TeV. The quoted limit uses a uniform positive prior in $1/\Lambda^2$.

10 AAD 13E limits are from $\mu^+\mu^-$ mass distribution in $pp$ collisions at $E_{cm} = 7$ TeV.

11 CHATRCHYAN 13K limits are from $\mu^+\mu^-$ mass distribution in $pp$ collisions at $E_{cm} = 7$ TeV.

12 AAD 12AB limits are from $\mu^+\mu^-$ mass distribution in $pp$ collisions at $E_{cm} = 7$ TeV.

SCALE LIMITS for Contact Interactions: $\Lambda(\ell\nu\ell\nu)$

<table><thead><tr><th>VALUE (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;3.10</strong></td><td>90</td><td>1 JODIDIO</td><td>86</td><td>SPEC Λ<sup>±</sup><sub>LR</sub>(ν<sub>μ</sub>ν<sub>e</sub>μ<sub>e</sub>)</td></tr></tbody></table>

1 JODIDIO 86 limit is from $\mu^+ \to \bar{\nu}_\mu e^+ e^-$. Chirality invariant interactions $L = (g^2/\Lambda^2)$ [$\eta_{LL}(\bar{\nu}_\mu L^\alpha \mu_L)(\bar{\ell}_L \gamma^\alpha e_L) + \eta_{LR}(\bar{\nu}_\mu L^\gamma \alpha e_L(\bar{R}_\gamma \alpha \mu_R)]$ with $g^2/4\pi = 1$ and $(\eta_{LL} \eta_{LR} = (0, \pm 1)$ are taken. No limits are given for $\Lambda_{LL}^{\pm}$ with $(\eta_{LL} \eta_{LR}) = (\pm 1, 0)$. For more general constraints with right-handed neutrinos and chirality nonconserving contact interactions, see their text.

2 DIAZCRUZ 94 limits are from $\Gamma(\tau \to e\nu\nu)$ and assume flavor-dependent contact interactions with $\Lambda(\tau\nu_\tau e\nu_e) \ll \Lambda(\mu\nu_\mu e\nu_e)$.

3 DIAZCRUZ 94 limits are from $\Gamma(\tau \to \mu\nu\nu)$ and assume flavor-dependent contact interactions with $\Lambda(\tau\nu_\tau \mu\nu_\mu) \ll \Lambda(\mu\nu_\mu e\nu_e)$.

SCALE LIMITS for Contact Interactions: $\Lambda(\ell e\nu q)$

<table><thead><tr><th>VALUE (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td><strong>&gt;2.81</strong></td><td>95</td><td>1 AFFOLDER</td><td>01I CDF</td></tr></tbody></table>

1 AFFOLDER 00I bound is for a scalar interaction $\bar{q}_R q_L \bar{\nu} e_L$.

SCALE LIMITS for Contact Interactions: $\Lambda(qqqq)$

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;13.1 none 17.4-29.5</strong></td><td><strong>&gt;21.8</strong></td><td>95</td><td>1 AABOUD</td><td>17AK ATLS</td><td>pp dijet angl.</td></tr></tbody></table>

1 AABOUD 17AK limit is from dijet angular distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV. u, d, and s quarks are assumed to be composite.

2 AABOUD 18W obtain limit on $t_R$ compositeness $2\pi/\Lambda_{RR}^2 < 1.6$ TeV$^{-2}$ at 95% CL from $t\bar{t}t\bar{t}$ production in the $pp$ collisions at $E_{cm} = 13$ TeV.

3 SIRUNYAN 18DD limit is from dijet angular distribution in $pp$ collisions at $\sqrt{s} = 13$ TeV.

4 SIRUNYAN 17F limit is from dijet angular cross sections in $pp$ collisions at $E_{cm} = 13$ TeV. All quarks are assumed to be composite.

5 AAD 16S limit is from dijet angular selections in $pp$ collisions at $E_{cm} = 13$ TeV. u, d, and s quarks are assumed to be composite.

6 AAD 15AR obtain limit on the $t_R$ compositeness $2\pi/\Lambda_{RR}^2 < 6.6$ TeV$^{-2}$ at 95% CL from the $t\bar{t}t\bar{t}$ production in the $pp$ collisions at $E_{cm} = 8$ TeV.

7 AAD 15BY obtain limit on the $t_R$ compositeness $2\pi/\Lambda_{RR}^2 < 15.1$ TeV$^{-2}$ at 95% CL from the $t\bar{t}t\bar{t}$ production in the $pp$ collisions at $E_{cm} = 8$ TeV.

8 AAD 15L limit is from dijet angular distribution in $pp$ collisions at $E_{cm} = 8$ TeV. u, d, s, c, and b quarks are assumed to be composite.

9 KHACHATRYAN 15J limit is from dijet angular distribution in $pp$ collisions at $E_{cm} = 8$ TeV. u, d, s, c, and b quarks are assumed to be composite.

10 FABBRICHESI 14 obtain bounds on chromoelectric and chromomagnetic form factors of the top-quark using $pp \to t\bar{t}$ and $p\bar{p} \to t\bar{t}$ cross sections. The quoted limit on the $q\bar{q}t\bar{t}$ contact interaction is derived from their bound on the chromoelectric form factor.

SCALE LIMITS for Contact Interactions: $\Lambda(\nu\nu qq)$

Limits are for $\Lambda_{LL}^{\pm}$ only. For other cases, see each reference.

<table><thead><tr><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>Λ<sup>+</sup><sub>LL</sub> (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;5.0</strong></td><td><strong>&gt;5.4</strong></td><td>95</td><td>1 MCFARLAND</td><td>98</td><td>CCFR νN scattering</td></tr></tbody></table>

1 MCFARLAND 98 assumed a flavor universal interaction. Neutrinos were mostly muon type.

MASS LIMITS for Excited e (e*)

Most $e^+e^-$ experiments assume one-photon or Z exchange. The limits from some $e^+e^-$ experiments which depend on λ have assumed transition couplings which are chirality violating ($\eta_L = \eta_R$). However they can be interpreted as limits for chirality-conserving interactions after multiplying the coupling value λ by $\sqrt{2}$; see Note.

Excited leptons have the same quantum numbers as other ortholeptons. See also the searches for ortholeptons in the “Searches for Heavy Leptons” section.

Limits for Excited e (e*) from Pair Production

These limits are obtained from $e^+e^- \to e^*e^-$ and thus rely only on the (elec- troweak) charge of $e^*$. Form factor effects are ignored unless noted. For the case of limits from Z decay, the $e^*$ coupling is assumed to be of sequential type. Possi- ble t channel contribution from transition magnetic coupling is neglected. All limits assume a dominant $e^* \to e\gamma$ decay except the limits from $\Gamma(Z)$.

For limits prior to 1987, see our 1992 edition (Physical Review D45 S1 (1992)).

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;103.2</strong></td><td>95</td><td>1 ABBIENDI</td><td>02G OPAL</td><td>e<sup>+</sup>e<sup>-</sup> → e<sup>*</sup>e<sup>*</sup> Homodoublet type</td></tr></tbody></table>

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

<table><tbody><tr><td>&gt;102.8</td><td>95</td><td>2 ACHARD</td><td>03B L3</td><td>e<sup>+</sup>e<sup>-</sup> → e<sup>*</sup>e<sup>*</sup> Homodoublet type</td></tr></tbody></table>

1 From $e^+e^-$ collisions at $\sqrt{s} = 183-209$ GeV, $f = f'$ is assumed.

2 From $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV, $f = f'$ is assumed. ACHARD 03B also obtain limit for $f = -f'$: $m_{e^*} > 96.6$ GeV.

Limits for Excited e (e*) from Single Production

These limits are from $e^+e^- \to e^*e$, $W \to e^*\nu$, or $ep \to e^*X$ and depend on transition magnetic coupling between $e$ and $e^*$. All limits assume $e^* \to e\gamma$ decay except as noted. Limits from LEP, UA2, and H1 are for chiral coupling, whereas all other limits are for nonchiral coupling, $\eta_L = \eta_R = 1$. In most papers, the limit is expressed in the form of an excluded region in the $\lambda-m_e^*$ plane. See the original papers.

For limits prior to 1987, see our 1992 edition (Physical Review D45 S1 (1992)).

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;5600</strong></td><td>95</td><td>1 SIRUNYAN</td><td>20AJ CMS</td><td>pp → ee<sup>*</sup> X</td></tr></tbody></table>

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

<table><tbody><tr><td>&gt;4800</td><td>95</td><td>2 AABOUD</td><td>19AZ ATLS</td><td>pp → ee<sup>*</sup> X</td></tr><tr><td>&gt;3900</td><td>95</td><td>3 SIRUNYAN</td><td>19Z CMS</td><td>pp → ee<sup>*</sup> X</td></tr><tr><td>&gt;2450</td><td>95</td><td>4 KHACHATRY...</td><td>16AQ CMS</td><td>pp → ee<sup>*</sup> X</td></tr><tr><td>&gt;3000</td><td>95</td><td>5 AAD</td><td>15AP ATLS</td><td>pp → e<sup>(*)</sup> e<sup>*</sup> X</td></tr><tr><td>&gt;2200</td><td>95</td><td>6 AAD</td><td>13BB ATLS</td><td>pp → ee<sup>*</sup> X</td></tr><tr><td>&gt;1900</td><td>95</td><td>7 CHATRCHYAN</td><td>13AE CMS</td><td>pp → ee<sup>*</sup> X</td></tr><tr><td>&gt;1870</td><td>95</td><td>8 AAD</td><td>12AZ ATLS</td><td>pp → e<sup>(*)</sup> e<sup>*</sup> X</td></tr></tbody></table>

1 SIRUNYAN 20AJ search for $e^*$ production in $2\pi\ell\gamma$ final states in $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit assumes $\Lambda = m_{e^*}$, $f = f' = 1$. The contact interaction is included. See their Fig.11 for exclusion limits in $m_{e^*} - \Lambda$ plane.

2 AABOUD 19AZ search for single $e^*$ production in $pp$ collisions at $\sqrt{s} = 13$ TeV. The limit quoted above is from $e^* \to eq\bar{q}$ and $e^* \to \nu W$ decays assuming $f = f' = 1$ and $m_{e^*} = \Lambda$. The contact interaction is included in $e^*$ production and decay amplitudes. See their Fig.6 for exclusion limits in $m_{e^*} - \Lambda$ plane.

3 SIRUNYAN 19Z search for $e^*$ production in $\ell\ell\gamma$ final states in $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit assumes $\Lambda = m_{e^*}$, $f = f' = 1$. The contact interaction is included in the $e^*$ production and decay amplitudes.

4 KHACHATRYAN 16AQ search for single $e^*$ production in $pp$ collisions at $\sqrt{s} = 8$ TeV. The limit above is from the $e^* \to e\gamma$ search channel assuming $f = f' = 1$, $m_{e^*} = \Lambda$. See their Table 7 for limits in other search channels or with different assumptions.
5 AAD 15AP search for $e^*e^*$ production in evens with three or more charged leptons in $pp$ collisions at $\sqrt{s} = 8$ TeV. The quoted limit assumes $\Lambda = m_{e^*}$, $f = f' = 1$. The contact interaction is included in the $e^*$ production and decay amplitudes.

6 AAD 13BB search for single $e^*$ production in $pp$ collisions with $e^* \to e\gamma$ decay. $f = f' = 1$, and $e^*$ production via contact interaction with $\Lambda = m_{e^*}$ are assumed.

7 CHATRCHYAN 13AE search for single $e^*$ production in $pp$ collisions with $e^* \to e\gamma$ decay. $f = f' = 1$, and $e^*$ production via contact interaction with $\Lambda = m_{e^*}$ are assumed.

8 AAD 12AZ search for $e^*$ production via four-fermion contact interaction in $pp$ collisions with $e^* \to e\gamma$ decay. The quoted limit assumes $\Lambda = m_{e^*}$. See their Fig. 8 for the exclusion plot in the mass-coupling plane.

### Limits for Excited $e$ ($e^*$) from $e^+e^- \to \gamma\gamma$

These limits are derived from indirect effects due to $e^*$ exchange in the $t$ channel and depend on transition magnetic coupling between $e$ and $e^*$. All limits are for $\lambda_\gamma = 1$. All limits except ABE 89j and ACHARD 02d are for nonchiral coupling with $\eta_L = \eta_R = 1$. We choose the chiral coupling limit as the best limit and list it in the Summary Table.

For limits prior to 1987, see our 1992 edition (Physical Review D45 S1 (1992)).

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;356</td><td>95</td><td>1 ABDALLAH</td><td>04N DLPH</td><td>$\sqrt{s}=161-208$ GeV</td></tr></tbody></table>

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

<table><tr><td>&gt;310</td><td>95</td><td>ACHARD</td><td>02D L3</td><td>$\sqrt{s}=192-209$ GeV</td></tr></table>

1 ABDALLAH 04N also obtain a limit on the excited electron mass with $e^e$ chiral coupling, $m_{e^*} > 295$ GeV at 95% CL.

### Indirect Limits for Excited $e$ ($e^*$)

These limits make use of loop effects involving $e^*$ and are therefore subject to theoretical uncertainty.

<table><thead><tr><th>VALUE (GeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td></td></tr></tbody></table>

1 DORENBOSCH... 89 CHRM $\bar{\nu}_{\mu}e \to \bar{\nu}_{\mu}e, \nu_{\mu}e \to \nu_{\mu}e$

2 GRIFOLS 86 THEO $\nu_{\mu}e \to \nu_{\mu}e$

3 RENARD 82 THEO $g-2$ of electron

1 DORENBOSCH 89 obtain the limit $\lambda_\gamma^2 \Lambda_{\text{cut}}^2/m_e^2 < 2.6$ (95% CL), where $\Lambda_{\text{cut}}$ is the cutoff scale, based on the one-loop calculation by GRIFOLS 86. If one assumes that $\Lambda_{\text{cut}} = 1$ TeV and $\lambda_\gamma = 1$, one obtains $m_{e^*} > 620$ GeV. However, one generally expects $\lambda_\gamma \approx m_{e^*}/\Lambda_{\text{cut}}$ in composite models.

2 GRIFOLS 86 uses $\nu_{\mu}e \to \nu_{\mu}e$ and $\bar{\nu}_{\mu}e \to \bar{\nu}_{\mu}e$ data from CHARM Collaboration to derive mass limits which depend on the scale of compositeness.

3 RENARD 82 derived from $g-2$ data limits on mass and couplings of $e^*$ and $\mu^*$. See figures 2 and 3 of the paper.

### MASS LIMITS for Excited $\mu$ ($\mu^*$)

#### Limits for Excited $\mu$ ($\mu^*$) from Pair Production

These limits are obtained from $e^+e^- \to \mu^+\mu^+\mu^-$ and thus rely only on the (elec- troweak) charge of $\mu^*$. Form factor effects are ignored unless noted. For the case of limits from $Z$ decay, the $\mu^*$ coupling is assumed to be of sequential type. All limits assume a dominant $\mu^* \to \mu\gamma$ decay except the limits from $\Gamma(Z)$.

For limits prior to 1987, see our 1992 edition (Physical Review D45 S1 (1992)).

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;103.2</td><td>95</td><td>1 ABBIENDI</td><td>02G OPAL</td><td>$e^+e^- \to \mu^+\mu^+\mu^*$ Homodouble type</td></tr></tbody></table>

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

<table><tr><td>&gt;102.8</td><td>95</td><td>2 ACHARD</td><td>03B L3</td><td>$e^+e^- \to \mu^+\mu^+\mu^*$ Homodouble type</td></tr></table>

1 From $e^+e^-$ collisions at $\sqrt{s} = 183-209$ GeV. $f = f'$ is assumed.

2 From $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV. $f = f'$ is assumed. ACHARD 03B also obtain limit for $f = -f'$: $m_{\mu^*} > 96.6$ GeV.

#### Limits for Excited $\mu$ ($\mu^*$) from Single Production

These limits are from $e^+e^- \to \mu^+\mu^+\mu^-$ and depend on transition magnetic coupling between $\mu$ and $\mu^*$. All limits assume $\mu^* \to \mu\gamma$ decay. Limits from LEP are for chiral coupling, whereas all other limits are for nonchiral coupling, $\eta_L = \eta_R = 1$. In most papers, the limit is expressed in the form of an excluded region in the $\lambda-m_{\mu^*}$ plane. See the original papers.

For limits prior to 1987, see our 1992 edition (Physical Review D45 S1 (1992)).

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;5700</td><td>95</td><td>1 SIRUNYAN</td><td>20AJ CMS</td><td>$pp \to \mu\mu^* X$</td></tr></tbody></table>

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

<table><tbody><tr><td>&gt;3800</td><td>95</td><td>2 SIRUNYAN</td><td>19Z CMS</td><td>$pp \to \mu\mu^* X$</td></tr><tr><td>&gt;2800</td><td>95</td><td>3 AAD</td><td>16BMATLS</td><td>$pp \to \mu\mu^* X$</td></tr><tr><td>&gt;2470</td><td>95</td><td>4 KHACHATRY...16AQ CMS</td><td>pp \to \mu\mu^* X</td><td></td></tr><tr><td>&gt;3000</td><td>95</td><td>5 AAD</td><td>15AP ATLS</td><td>$pp \to \mu^*(\mu^*) X$</td></tr><tr><td>&gt;2200</td><td>95</td><td>6 AAD</td><td>13BB ATLS</td><td>$pp \to \mu\mu^* X$</td></tr><tr><td>&gt;1900</td><td>95</td><td>7 CHATRCHYAN 13AE CMS</td><td>pp \to \mu\mu^* X</td><td></td></tr><tr><td>&gt;1750</td><td>95</td><td>8 AAD</td><td>12AZ ATLS</td><td>$pp \to \mu^*(\mu^*) X$</td></tr></tbody></table>

1 SIRUNYAN 20AJ search for $\mu^*$ production in $2\mu2j$ final states in $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit assumes $\Lambda = m_{\mu^*}$, $f = f' = 1$. The contact interaction is included. See their Fig.11 for exclusion limits in $m_{\mu^*}-\Lambda$ plane.

2 SIRUNYAN 19Z search for $\mu^*$ production in $\ell\ell\gamma$ final states in $pp$ collisions at $\sqrt{s} = 13$ TeV. The quoted limit assumes $\Lambda = m_{\mu^*}$, $f = f' = 1$. The contact interaction is included in the $\mu^*$ production and decay amplitudes.

3 AAD 16BM search for $\mu^*$ production in $\mu\mu\mu j$ events in $pp$ collisions at $\sqrt{s} = 8$ TeV. Both the production and decay are assumed to occur via a contact interaction with $\Lambda = m_{\mu^*}$.

4 KHACHATRYAN 16AQ search for single $\mu^*$ production in $pp$ collisions at $\sqrt{s} = 8$ TeV. The limit above is from the $\mu^* \to \mu\gamma$ search channel assuming $f = f' = 1$, $m_{\mu^*} = \Lambda$. See their Table 7 for limits in other search channels or with different assumptions.

5 AAD 15AP search for $\mu^*$ production in evens with three or more charged leptons in $pp$ collisions at $\sqrt{s} = 8$ TeV. The quoted limit assumes $\Lambda = m_{\mu^*}$, $f = f' = 1$. The contact interaction is included in the $\mu^*$ production and decay amplitudes.

6 AAD 13BB search for single $\mu^*$ production in $pp$ collisions with $\mu^* \to \mu\gamma$ decay, $f = f' = 1$, and $\mu^*$ production via contact interaction with $\Lambda = m_{\mu^*}$ are assumed.

7 CHATRCHYAN 13AE search for single $\mu^*$ production in $pp$ collisions with $\mu^* \to \mu\gamma$ decay, $f = f' = 1$, and $\mu^*$ production via contact interaction with $\Lambda = m_{\mu^*}$ are assumed.

8 AAD 12AZ search for $\mu^*$ production via four-fermion contact interaction in $pp$ collisions with $\mu^* \to \mu\gamma$ decay. The quoted limit assumes $\Lambda = m_{\mu^*}$. See their Fig. 8 for the exclusion plot in the mass-coupling plane.

### Indirect Limits for Excited $\mu$ ($\mu^*$)

These limits make use of loop effects involving $\mu^*$ and are therefore subject to theoretical uncertainty.

<table><thead><tr><th>VALUE (GeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td></td></tr></tbody></table>

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

1 RENARD 82 THEO $g-2$ of muon

1 RENARD 82 derived from $g-2$ data limits on mass and couplings of $e^*$ and $\mu^*$. See figures 2 and 3 of the paper.

### MASS LIMITS for Excited $\tau$ ($\tau^*$)

#### Limits for Excited $\tau$ ($\tau^*$) from Pair Production

These limits are obtained from $e^+e^- \to \tau^+\tau^+\tau^-$ and thus rely only on the (elec- troweak) charge of $\tau^*$. Form factor effects are ignored unless noted. For the case of limits from $Z$ decay, the $\tau^*$ coupling is assumed to be of sequential type. All limits assume a dominant $\tau^* \to \tau\gamma$ decay except the limits from $\Gamma(Z)$.

For limits prior to 1987, see our 1992 edition (Physical Review D45 S1 (1992)).

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;103.2</td><td>95</td><td>1 ABBIENDI</td><td>02G OPAL</td><td>$e^+e^- \to \tau^*\tau^* \text{ Homodouble type}$</td></tr></tbody></table>

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

<table><tr><td>&gt;102.8</td><td>95</td><td>2 ACHARD</td><td>03B L3</td><td>$e^+e^- \to \tau^*\tau^* \text{ Homodouble type}$</td></tr></table>

1 From $e^+e^-$ collisions at $\sqrt{s} = 183-209$ GeV. $f = f'$ is assumed.

2 From $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV. $f = f'$ is assumed. ACHARD 03B also obtain limit for $f = -f'$: $m_{\tau^*} > 96.6$ GeV.

#### Limits for Excited $\tau$ ($\tau^*$) from Single Production

These limits are from $e^+e^- \to \tau^+\tau^+$ and depend on transition magnetic coupling between $\tau$ and $\tau^*$. All limits assume $\tau^* \to \tau\gamma$ decay. Limits from LEP are for chiral coupling, whereas all other limits are for nonchiral coupling, $\eta_L = \eta_R = 1$. In most papers, the limit is expressed in the form of an excluded region in the $\lambda-m_{\tau^*}$ plane. See the original papers.

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;4600</td><td>95</td><td>1 AAD</td><td>23BJ ATLS</td><td>$pp \to \tau\tau^*$</td></tr></tbody></table>

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

<table><tr><td>&gt;2500</td><td>95</td><td>2 AAD</td><td>15AP ATLS</td><td>$pp \to \tau^*(\mu^*) \tau^* X$</td></tr></table>

<table><tr><td>&gt; 180</td><td>95</td><td>3 ACHARD</td><td>03B L3</td><td>$e^+e^- \to \tau\tau^*$</td></tr></table>

<table><tr><td>&gt; 185</td><td>95</td><td>4 ABBIENDI</td><td>02G OPAL</td><td>$e^+e^- \to \tau\tau^*$</td></tr></table>

1 AAD 23BJ search for $\tau^*$ produced in association with $\tau$ and decaying into $\tau q\bar{q}$ via a contact interaction with $g^2_{\text{contact}} = (4\pi)^2$. The limit quoted above assumes $\Lambda = m_{\tau^*}$.

2 AAD 15AP search for $\tau^*$ production in events with three or more charged leptons in $pp$ collisions at $\sqrt{s} = 8$ TeV. The quoted limit assumes $\Lambda = m_{\tau^*}$, $f = f' = 1$. The contact interaction is included in the $\tau^*$ production and decay amplitudes.

3 ACHARD 03B result is from $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV. $f = f' = \Lambda/m_{\tau^*}$ is assumed. See their Fig. 4 for the exclusion plot in the mass-coupling plane.

4 ABBIENDI 02G result is from $e^+e^-$ collisions at $\sqrt{s} = 183-209$ GeV. $f = f' = \Lambda/m_{\tau^*}$ is assumed for $\tau^*$ coupling. See their Fig. 4c for the exclusion limit in the mass-coupling plane.

### MASS LIMITS for Excited Neutrino ($\nu$*)

#### Limits for Excited $\nu$ ($\nu^*$) from Pair Production

These limits are obtained from $e^+e^- \to \nu^*\nu^*$ and thus rely only on the (electroweak) charge of $\nu^*$. Form factor effects are ignored unless noted. The $\nu^*$ coupling is assumed to be of sequential type unless otherwise noted. All limits assume a dominant $\nu^* \to \nu\gamma$ decay except the limits from $\Gamma(Z)$.

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;1600</td><td>95</td><td>1 AAD</td><td>15AP ATLS</td><td>$pp \to \nu^*\nu^* X$</td></tr></tbody></table>
• • • We do not use the following data for averages, fits, limits, etc. • • •

2 ABBIENDI 04N OPAL
> 102.6 95 3 ACHARD 03B L3 e⁺e⁻ → ν⁺ν⁻ Homodoublet type

1 AAD 15AP search for ν⁺ pair production in events with three or more charged leptons in $pp$ collisions at $\sqrt{s} = 8$ TeV. The quoted limit assumes $\Lambda = m_{\nu^+}$, $f = f' = 1$. The contact interaction is included in the $\nu^+$ production and decay amplitudes.

2 From $e^+e^-$ collisions at $\sqrt{s} = 192-209$ GeV, ABBIENDI 04N obtain limit on $\sigma(e^+e^- \to \nu^+\nu^-) B^2(\nu^+ \to \nu\gamma)$. See their Fig.2. The limit ranges from 20 to 45 fb for $m_{\nu^+} > 45$ GeV.

3 From $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV, $f = -f'$ is assumed. ACHARD 03B also obtain limit for $f = f'$: $m_{\nu_e^+} > 101.7$ GeV, $m_{\nu_\mu^+} > 101.8$ GeV, and $m_{\nu_T^+} > 92.9$ GeV. See their Fig. 4 for the exclusion plot in the mass-coupling plane.

### Limits for Excited $\nu$ ($\nu^*$) from Single Production

These limits are from $e^+e^- \to \nu\nu^*$, $Z \to \nu\nu^*$, or $e p \to \nu^* X$ and depend on transition magnetic coupling between $\nu$ and $\nu^*$. Assumptions about $\nu^*$ decay mode are given in footnotes.

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt; 213</td><td>95</td><td>1 AARON</td><td>08</td><td>e p → ν<sup>*</sup> X</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>>6000</td><td>95</td><td>2 TUMASYAN</td><td>23AL CMS</td><td>pp → ℓν<sup>*</sup> → ℓℓqq, ℓ = e</td></tr><tr><td>> 190</td><td>95</td><td>3 ACHARD</td><td>03B L3</td><td>e<sup>+</sup>e<sup>-</sup> → νν<sup>*</sup>ν</td></tr><tr><td>none 50-150</td><td>95</td><td>4 ADLOFF</td><td>02 H1</td><td>e p → ν<sup>*</sup> X</td></tr><tr><td>> 158</td><td>95</td><td>5 CHEKANOV</td><td>02D ZEUS</td><td>e p → ν<sup>*</sup> X</td></tr></tbody></table>

1 AARON 08 search for single $\nu^*$ production in $e p$ collisions with the decays $\nu^* \to \nu\gamma$, $\nu Z$, $e W$. The quoted limit assumes $f = -f' = \Lambda/m_{\nu^*}$. See their Fig. 3 and Fig. 4 for the exclusion plots in the mass-coupling plane.

2 TUMASYAN 23AL search for Majorana excited neutrino $\nu^*$ produced and decaying via gauge and contact interactions. The limit quoted above is for $\ell = e$ with $\Lambda = M_{\nu^*}$. The limit becomes $M_{\nu^*} > 6.1$ TeV for $\ell = \mu$.

3 ACHARD 03B result is from $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV. The quoted limit is for $\nu_e^*$, $f = -f' = \Lambda/m_{\nu_e^*}$, is assumed. See their Fig. 4 for the exclusion plot in the mass-coupling plane.

4 ADLOFF 02 search for single $\nu^*$ production in $e p$ collisions with the decays $\nu^* \to \nu\gamma$, $\nu Z$, $e W$. The quoted limit assumes $f = -f' = \Lambda/m_{\nu^*}$. See their Fig. 1 for the exclusion plots in the mass-coupling plane.

5 CHEKANOV 02d search for single $\nu^*$ production in $e p$ collisions with the decays $\nu^* \to \nu\gamma$, $\nu Z$, $e W$, $f = -f' = \Lambda/m_{\nu^*}$ is assumed for the $e^+$ coupling. CHEKANOV 02d also obtain limit for $f = f' = \Lambda/m_{\nu^*}$: $m_{\nu_e^*} > 135$ GeV. See their Fig. 5c and Fig. 5d for the exclusion plot in the mass-coupling plane.

### MASS LIMITS for Excited $q$ ($q^*$)

#### Limits for Excited $q$ ($q^*$) from Pair Production

These limits are mostly obtained from $e^+e^- \to q^* q^*$ and thus rely only on the (elec- troweak) charge of the $q^*$. Form factor effects are ignored unless noted. Assumptions about the $q^*$ decay are given in the comments and footnotes.

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;338</td><td>95</td><td>1 AALTONEN</td><td>10H CDF</td><td>q* → tW<sup>-</sup></td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>none 700-1200</td><td>95</td><td>2 SIRUNYAN</td><td>18V CMS</td><td>pp → t<sup>*</sup><sub>3/2</sub> t<sup>*</sup><sub>3/2</sub> → t<span style="text-decoration: overline">t</span>g g</td></tr><tr><td>> 45.6</td><td>95</td><td>3 BARATE</td><td>98U ALEP</td><td>Z → q<sup>*</sup> q<sup>*</sup></td></tr><tr><td>> 41.7</td><td>95</td><td>4 ADRIANI</td><td>93M L3</td><td>u or d type, Z → q<sup>*</sup> q<sup>*</sup></td></tr><tr><td>> 44.7</td><td>95</td><td>5 BARDADIN...</td><td>92 RVUE</td><td>u-type, Γ(Z)</td></tr><tr><td>> 40.6</td><td>95</td><td>5 BARDADIN...</td><td>92 RVUE</td><td>d-type, Γ(Z)</td></tr><tr><td>> 44.2</td><td>95</td><td>6 DECAMP</td><td>92 ALEP</td><td>u-type, Γ(Z)</td></tr><tr><td>> 45</td><td>95</td><td>6 DECAMP</td><td>92 ALEP</td><td>d-type, Γ(Z)</td></tr><tr><td>> 45</td><td>95</td><td>7 DECAMP</td><td>92 ALEP</td><td>u or d type, Z → q<sup>*</sup> q<sup>*</sup></td></tr><tr><td>> 45</td><td>95</td><td>6 ABREU</td><td>91F DLPH</td><td>u-type, Γ(Z)</td></tr><tr><td>> 45</td><td>95</td><td>6 ABREU</td><td>91F DLPH</td><td>d-type, Γ(Z)</td></tr></tbody></table>

1 AALTONEN 10h obtain limits on the $q^* q^*$ production cross section in $p\bar{p}$ collisions. See their Fig. 3.

2 SIRUNYAN 18V search for pair production of spin 3/2 excited top quarks. $B(t^{*3/2} \to tg) = 1$ is assumed.

3 BARATE 98U obtain limits on the form factor. See their Fig. 16 for limits in mass-form factor plane.

4 ADRIANI 93M limit is valid for $B(q^* \to qg) > 0.25$ (0.17) for up (down) type.

5 BARDADIN-OTWINOWSKA 92 limit based on $\Delta\Gamma(Z) < 36$ MeV.

6 These limits are independent of decay modes.

7 Limit is for $B(q^* \to qg) + B(q^* \to q\gamma) = 1$.

#### Limits for Excited $q$ ($q^*$) from Single Production

These limits are from $e^+e^- \to q^* q$, $p\bar{p} \to q^* X$, or $pp \to q^* X$ and depend on transition magnetic couplings between $q$ and $q^*$. Assumptions about $q^*$ decay mode are given in the footnotes and comments.

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;6700 (CL = 95%)</td><td></td><td></td><td></td><td></td></tr><tr><td>none 1800-2500</td><td>95</td><td>1 TUMASYAN</td><td>23AL CMS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → bg</td></tr><tr><td>none 1000-6000</td><td>95</td><td>2 TUMASYAN</td><td>23BC CMS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qγ</td></tr></tbody></table>

<table><tbody><tr><td>none 1000-2200</td><td>95</td><td>3 TUMASYAN</td><td>23BC CMS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → bγ</td></tr><tr><td>none 2000-6700</td><td>95</td><td>4 AAD</td><td>20T ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → bg</td></tr><tr><td>none 1250-3200</td><td>95</td><td>4 AAD</td><td>20T ATLS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → bg, bγ, bZ, tW</td></tr><tr><td>none 1800-6300</td><td>95</td><td>5 SIRUNYAN</td><td>20AI CMS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → bg</td></tr><tr><td>none 1500-2600</td><td>95</td><td>6 AABOUD</td><td>18AB ATLS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → bg</td></tr><tr><td>none 1500-5300</td><td>95</td><td>7 AABOUD</td><td>18BA ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qγ</td></tr><tr><td>none 1000-5500</td><td>95</td><td>8 SIRUNYAN</td><td>18AG CMS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qγ</td></tr><tr><td>none 1000-1800</td><td>95</td><td>9 SIRUNYAN</td><td>18AG CMS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → bγ</td></tr><tr><td>none 600-6000</td><td>95</td><td>10 SIRUNYAN</td><td>18B0 CMS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr><tr><td>none 1200-5000</td><td>95</td><td>11 SIRUNYAN</td><td>18P CMS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qW</td></tr><tr><td>none 1200-4700</td><td>95</td><td>11 SIRUNYAN</td><td>18P CMS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qZ</td></tr><tr><td>>6000</td><td>95</td><td>12 AABOUD</td><td>17AK ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr></tbody></table>

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

<table><tbody><tr><td>none 700-3000</td><td>95</td><td>13 TUMASYAN</td><td>220 CMS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → tW</td></tr><tr><td>>2600</td><td>95</td><td>14 SIRUNYAN</td><td>21AG CMS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → tW</td></tr><tr><td>none 600-5400</td><td>95</td><td>15 KHACHATRY...17W CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr><tr><td>none 1100-2100</td><td>95</td><td>16 AABOUD</td><td>16 ATLS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → bg</td></tr><tr><td>>1500</td><td>95</td><td>17 AAD</td><td>16AH ATLS</td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → tW</td></tr><tr><td>>4400</td><td>95</td><td>18 AAD</td><td>16AI ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qγ</td></tr><tr><td></td><td></td><td>19 AAD</td><td>16AV ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → Wb</td></tr><tr><td>>5200</td><td>95</td><td>20 AAD</td><td>16S ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr><tr><td>>1390</td><td>95</td><td>21 KHACHATRY...16I CMS</td><td></td><td>pp → b<sup>*</sup> X, b<sup>*</sup> → tW</td></tr><tr><td>>5000</td><td>95</td><td>22 KHACHATRY...16K CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr><tr><td>none 500-1600</td><td>95</td><td>23 KHACHATRY...16L CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr><tr><td>>4060</td><td>95</td><td>24 AAD</td><td>15V ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr><tr><td>>3500</td><td>95</td><td>25 KHACHATRY...15V CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qg</td></tr><tr><td>>3500</td><td>95</td><td>26 AAD</td><td>14A ATLS</td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qγ</td></tr><tr><td>>3200</td><td>95</td><td>27 KHACHATRY...14 CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qW</td></tr><tr><td>>2900</td><td>95</td><td>28 KHACHATRY...14 CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qZ</td></tr><tr><td>none 700-3500</td><td>95</td><td>29 KHACHATRY...14J CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qγ</td></tr><tr><td>>2380</td><td>95</td><td>30 CHATRCHYAN 13AJ CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qW</td></tr><tr><td>>2150</td><td>95</td><td>31 CHATRCHYAN 13AJ CMS</td><td></td><td>pp → q<sup>*</sup> X, q<sup>*</sup> → qZ</td></tr></tbody></table>

1 TUMASYAN 23AF limit quoted above assumes $bg \to b^*$ production. The limit becomes $m_{b^*} > 4$ TeV if contact interaction is included in the $b^*$ production cross section. See their Fig. 5 for limits on $\sigma \cdot B$.

2 TUMASYAN 23BC search for excited light flavor quark $q^*$ in $pp$ collisions at $\sqrt{s} = 13$ TeV, $f = 1.0$ is assumed.

3 TUMASYAN 23BC search for excited b quark $b^*$ in $pp$ collisions at $\sqrt{s} = 13$ TeV, $b^*$ production via gauge interactions and $f = 1.0$ are assumed. The limit becomes $m_{b^*} > 3.8$ TeV if contact interaction is included in the $b^*$ production cross section.

4 AAD 20T search for resonances decaying into dijets in $pp$ collisions at $\sqrt{s} = 13$ TeV. Assume $\Lambda = m_{q^*}$, $f_S = f = f' = 1$.

5 SIRUNYAN 20AI search for resonances decaying into dijets in $pp$ collisions at $\sqrt{s} = 13$ TeV. Assume $\Lambda = m_{q^*}$, $f_S = f = f' = 1$.

6 AABOUD 18AB assume $\Lambda = m_{b^*}$, $f_S = f = f' = 1$. The contact interactions are not included in $b^*$ production and decay amplitudes.

7 AABOUD 18BA search for first-generation excited quarks ($u^*$ and $d^*$) with degenerate mass, assuming $\Lambda = m_{q^*}$, $f_S = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes.

8 SIRUNYAN 18AG search for first-generation excited quarks ($u^*$ and $d^*$) with degenerate mass, assuming $\Lambda = m_{q^*}$, $f_S = f = f' = 1$.

9 SIRUNYAN 18AG search for excited b quark assuming $\Lambda = m_{q^*}$, $f_S = f = f' = 1$.

10 SIRUNYAN 18B0 assume $\Lambda = m_{q^*}$, $f_S = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes.

11 SIRUNYAN 18P use the hadronic decay of $W$ or $Z$, assuming $\Lambda = m_{q^*}$, $f_S = f = f' = 1$.

12 AABOUD 17AK assume $\Lambda = m_{q^*}$, $f_S = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes. Only the decay of $q^* \to g u$ and $q^* \to g d$ is simulated as the benchmark signals in the analysis.

13 TUMASYAN 22O search for $b^*$ decaying to $tW$ in $pp$ collisions at $\sqrt{s} = 13$ TeV. The limit quoted above assumes $\kappa_L^b = g_L = 1$, $\kappa_R^b = g_R = 0$. The limit becomes $m_{b^*} > 3.0$ TeV (>3.2 TeV) if we assume $\kappa_L^b = g_L = 0$, $\kappa_R^b = g_R = 1$ ($\kappa_L^b = g_L = 1$, $\kappa_R^b = g_R = 1$). See their Fig. 3 for limits on $\sigma \cdot B$.

14 SIRUNYAN 21AG search for $b^*$ decaying to $tW$ in $pp$ collisions at $\sqrt{s} = 13$ TeV. The limit quoted above assumes $\kappa_L^b = g_L = 1$, $\kappa_R^b = g_R = 0$. The limit becomes $m_{b^*} > 2.8$ TeV (>3.1 TeV) if we assume $\kappa_L^b = g_L = 0$, $\kappa_R^b = g_R = 1$ ($\kappa_L^b = g_L = 1$, $\kappa_R^b = g_R = 1$). See their Fig. 5 for limits on $\sigma \cdot B$.

15 KHACHATRYAN 17W assume $\Lambda = m_{q^*}$, $f_S = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes.

16 AABOUD 16AG assume $\Lambda = m_{b^*}$, $f_S = f = f' = 1$. The contact interactions are not included in the $b^*$ production and decay amplitudes.

17 AAD 16AH search for $b^*$ decaying to $tW$ in $pp$ collisions at $\sqrt{s} = 8$ TeV. $f_g = f_L = f_R = 1$ are assumed. See their Fig. 12b for limits on $\sigma \cdot B$.

18 AAD 16AI assume $\Lambda = m_{q^*}$, $f_S = f = f' = 1$.

19 AAD 16AV search for single production of vector-like quarks decaying to $Wb$ in $pp$ collisions. See their Fig. 8 for the limits on couplings and mixings.

20 AAD 16S assume $\Lambda = m_{q^*}$, $f_S = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes.
21 KHACHATRYAN 16l search for b\* decaying to tW in $pp$ collisions at $\sqrt{s} = 8$ TeV, $\kappa_L^b = g_L = 1$, $\kappa_R^b = g_R = 0$ are assumed. See their Fig. 8 for limits on $\sigma \cdot B$.

22 KHACHATRYAN 16k assume $\Lambda = m_q^*$, $f_s = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes.

23 KHACHATRYAN 16l search for resonances decaying to dijets in $pp$ collisions at $\sqrt{s} = 8$ TeV using the data scouting technique which increases the sensitivity to the low mass resonances.

24 AAD 15v assume $\Lambda = m_q^*$, $f_s = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes.

25 KHACHATRYAN 15v assume $\Lambda = m_q^*$, $f_s = f = f' = 1$. The contact interactions are not included in $q^*$ production and decay amplitudes.

26 AAD 14a assume $\Lambda = m_q^*$, $f_s = f = f' = 1$.

27 KHACHATRYAN 14 use the hadronic decay of W, assuming $\Lambda = m_q^*$, $f_s = f = f' = 1$.

28 KHACHATRYAN 14 use the hadronic decay of Z, assuming $\Lambda = m_q^*$, $f_s = f = f' = 1$.

29 KHACHATRYAN 14j assume $f_s = f = f' = \Lambda / m_q^*$.

30 CHATRYCHYAN 13aJ use the hadronic decay of W.

31 CHATRYCHYAN 13aJ use the hadronic decay of Z.

### MASS LIMITS for Color Sextet Quarks ($\ell_6$)

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>>84</td><td>95</td><td>1 ABE</td><td>89d</td><td>$p\bar{p} \to \ell_6\bar{\ell}_6$</td></tr></tbody></table>

1 ABE 89d look for pair production of unit-charged particles which leave the detector before decaying. In the above limit the color sextet quark is assumed to fragment into a unit-charged or neutral hadron with equal probability and to have long enough lifetime not to decay within the detector. A limit of 121 GeV is obtained for a color decuplet.

### MASS LIMITS for Color Octet Charged Leptons ($\ell_8$)

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>>86</td><td>95</td><td>1 ABE</td><td>89d</td><td>$\text{Stable } \ell_8: p\bar{p} \to \ell_8\bar{\ell}_8$</td></tr></tbody></table>

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

2 ABT 93 H1 $e_g: e_p \to e_g X$

1 ABE 89d look for pair production of unit-charged particles which leave the detector before decaying. In the above limit the color octet lepton is assumed to fragment into a unit-charged or neutral hadron with equal probability and to have long enough lifetime not to decay within the detector. The limit improves to 99 GeV if it always fragments into a unit-charged hadron.

2 ABT 93 search for $e_8$ production via e-gluon fusion in $e\bar{p}$ collisions with $e_8 \to e g$. See their Fig. 3 for exclusion plot in the $m_{e_8} - \Lambda$ plane for $m_{e_8} = 35-220$ GeV.

### MASS LIMITS for Color Octet Neutrinos ($\nu_8$)

<table><thead><tr><th>VALUE (GeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>>110</td><td>90</td><td>1 BARGER</td><td>89</td><td>$\text{RVUE } \nu_8: p\bar{p} \to \nu_8\bar{\nu}_8$</td></tr></tbody></table>

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

none 3.8-29.8 95 2 KIM 90 AMY $\nu_8: e^+ e^- \to \text{acoplanar jets}$

none 9-21.9 95 3 BARTEL 87b JADE $\nu_8: e^+ e^- \to \text{acoplanar jets}$

1 BARGER 89 used ABE 89b limit for events with large missing transverse momentum. Two-body decay $\nu_8 \to \nu g$ is assumed.

2 KIM 90 is at $E_{cm} = 50-60$ GeV. The same assumptions as in BARTEL 87b are used.

3 BARTEL 87b is at $E_{cm} = 46.3-46.78$ GeV. The limit assumes the $\nu_8$ pair production cross section to be eight times larger than that of the corresponding heavy neutrino pair production. This assumption is not valid in general for the weak couplings, and the limit can be sensitive to its $SU(2)_L \times U(1)_Y$ quantum numbers.

### MASS LIMITS for $W_8$ (Color Octet W Boson)

<table><thead><tr><th>VALUE (GeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody></tbody></table>

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

1 ALBAJAR 89 UA1 $p\bar{p} \to W_8 X$, $W_8 \to W g$
1 ALBAJAR 89 give $\sigma(W_8 \to W + jet)/\sigma(W) < 0.019$ (90% CL) for $m_{W_8} > 220$ GeV.

### REFERENCES FOR Searches for Quark and Lepton Compositeness

<table><tr><td>AAD</td><td>23BJ JHEP 2306, 199</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23AF PR D108 012009</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23AL PL B843 137803</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>23BC JHEP 2312 189</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>TUMASYAN</td><td>22O JHEP 2204 048</td><td>A. Tumasyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>21AU PRL 127 148011</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>21Q JHEP 2104 142</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21AG JHEP 2112 106</td><td>A. M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>21N JHEP 2107 208</td><td>A. M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>20AP JHEP 2011 005</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>20T JHEP 2003 145</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20AI JHEP 2005 033</td><td>A. M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>20AJ JHEP 2005 052</td><td>A. M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AABOUD</td><td>19AZ EPJ C79 803</td><td>M. Aadoub et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>ABRAMOWICZ</td><td>19 PR D99 092006</td><td>H. Abramowicz et al.</td><td>(ZEUS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19AC JHEP 1904 114</td><td>A. M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>19Z JHEP 1904 015</td><td>A. M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AABOUD</td><td>18AB PR D98 032016</td><td>M. Aadoub et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>18AV JHEP 1807 089</td><td>M. Aadoub et al.</td><td>(CMS Collab.)</td></tr><tr><td>AABOUD</td><td>18BA EPJ C78 102</td><td>M. Aadoub et al.</td><td>(ATLAS Collab.)</td></tr></table>

<table><tr><td>SIRUNYAN</td><td>18AG PL B781 390</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18BO JHEP 1808 130</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18DD EPJ C78 789</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18P PR D97 027006</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>18V PL B788 349</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AABOUD</td><td>17AK PR D96 052004</td><td>M. Aadoub et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>17AT JHEP 1710 182</td><td>M. Aadoub et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>KHACHATRYAN</td><td>17W PL B769 520</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>SIRUNYAN</td><td>17F JHEP 1707 013</td><td>A.M. Sirunyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AABOUD</td><td>16 PL B759 229</td><td>M. Aadoub et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AABOUD</td><td>16U PL B761 372</td><td>M. Aadoub et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16AH JHEP 1603 110</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16AI JHEP 1603 041</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16AV EPJ C76 442</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16BM NJP 18 073021</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>16S PL B754 302</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>KHACHATRYAN</td><td>16AQ JHEP 1603 125</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>KHACHATRYAN</td><td>16I JHEP 1601 166</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>KHACHATRYAN</td><td>16K PRL 116 071801</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>KHACHATRYAN</td><td>16L PRL 117 031802</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>15AP JHEP 1508 138</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15AR JHEP 1508 105</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15AY JHEP 1510 150</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15L PRL 114 221802</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>15V PR D91 052007</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>KHACHATRY</td><td>15AE JHEP 1504 025</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>KHACHATRY</td><td>15J PRL B746 79</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>KHACHATRY</td><td>15V PR D91 052009</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>14A PL B728 562</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>14BE EPJ C74 3134</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>FABBRICHESI</td><td>14 PR D89 074028</td><td>M. Fabbrichesi, M. Pinamonti, A. Tonero</td><td>(CMS Collab.)</td></tr><tr><td>KHACHATRY</td><td>14 JHEP 1408 173</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>KHACHATRY</td><td>14J PL B738 274</td><td>V. Khachatryan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>13BB NJP 0930111</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>13E PR D87 015010</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYCHYAN</td><td>13AE PL B720 309</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYCHYAN</td><td>13AJ PL B723 280</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>CHATRYCHYAN</td><td>13K PR D87 032001</td><td>S. Chatrchyan et al.</td><td>(CMS Collab.)</td></tr><tr><td>AAD</td><td>12BB JHEP 1212 40</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AAD</td><td>12AZ PR D85 072003</td><td>G. Aad et al.</td><td>(ATLAS Collab.)</td></tr><tr><td>AARON</td><td>11C PL B705 52</td><td>F. D. Aaron et al.</td><td>(H1 Collab.)</td></tr><tr><td>ABDALLAH</td><td>11 EPJ C71 1555</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>AALTONEN</td><td>10H PRL 104 091801</td><td>T. Aaltonen et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABDALLAH</td><td>09 PL B560 1</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>AARON</td><td>08 PL B663 382</td><td>F.D. Aaron et al.</td><td>(H1 Collab.)</td></tr><tr><td>SCHAEL</td><td>07A EPJ C49 411</td><td>S. Schael et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>ABDALLAH</td><td>06C EPJ C45 589</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ABULENCIA</td><td>06L PRL 96 211801</td><td>A. Abulencia et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABBIENDI</td><td>04G EPJ C33 173</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABBIENDI</td><td>04N PL B602 167</td><td>G. Abbiendi et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABDALLAH</td><td>04N EPJ C37 405</td><td>J. Abdallah et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>ACHARD</td><td>03B PL B568 23</td><td>P. Acard et al.</td><td>(L3 Collab.)</td></tr><tr><td>BABICH</td><td>03 EPJ C29 103</td><td>A.A. Babich et al.</td><td>(OPAL Collab.)</td></tr><tr><td>ABBIENDI</td><td>02G PL B544 57</td><td>G. Abbiendi et al.</td><td>(L3 Collab.)</td></tr><tr><td>ACHARD</td><td>02D PL B531 28</td><td>P. Acard et al.</td><td>(H1 Collab.)</td></tr><tr><td>ADLOFF</td><td>02 PL B525 9</td><td>C. Adloff et al.</td><td>(CDF Collab.)</td></tr><tr><td>CHEKANOV</td><td>02D PL B549 32</td><td>S. Chekanov et al.</td><td>(ZEUS Collab.)</td></tr><tr><td>AFFOLDER</td><td>01I PRL 87 231803</td><td>T. Affolder et al.</td><td>(CDF Collab.)</td></tr><tr><td>BOURILKOV</td><td>01I PR D64 071701</td><td>D. Bourilkov</td><td>(L3 Collab.)</td></tr><tr><td>CHEUNG</td><td>00P PL B517 167</td><td>K. Cheung</td><td>(L3 Collab.)</td></tr><tr><td>ACCIARRI</td><td>00B PL B489 81</td><td>M. Acciarr et al.</td><td>(CDF Collab.)</td></tr><tr><td>AFFOLDER</td><td>001 PR D62 012004</td><td>T. Affolder et al.</td><td>(L3 Collab.)</td></tr><tr><td>BARATE</td><td>98U EPJ C4 571</td><td>R. Barate et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>BARGER</td><td>98E EPJ D57 391</td><td>V. Barger et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>MCFARLAND</td><td>98 EPJ C1 509</td><td>V. Barger et al.</td><td>(CCFR/NuTeV Collab.)</td></tr><tr><td>DIAZCRUZ</td><td>94 PR D9 2149</td><td>J.L. Diaz Cruz, O.A. Sampayo</td><td>(CINV Collab.)</td></tr><tr><td>ABT</td><td>93 NP B396 3</td><td>I. Abt et al.</td><td>(H1 Collab.)</td></tr><tr><td>ADRIANI</td><td>93M PRPL 236 1</td><td>O. Adriani et al.</td><td>(L3 Collab.)</td></tr><tr><td>BARBIADIN...</td><td>92 ZPHY C55 163</td><td>M. Bardadin-Otwinowska</td><td>(CLER Collab.)</td></tr><tr><td>DECAMP</td><td>92 PRL 216 253</td><td>D. Decamp et al.</td><td>(ALEPH Collab.)</td></tr><tr><td>PDG</td><td>92 PR D45 51</td><td>K. Hikasa et al.</td><td>(KEK, LBL, BOST+)</td></tr><tr><td>ABREU</td><td>91F NP B367 511</td><td>P. Abreu et al.</td><td>(DELPHI Collab.)</td></tr><tr><td>KIM</td><td>90 PL B240 243</td><td>G.N. Kim et al.</td><td>(AMY Collab.)</td></tr><tr><td>ABE</td><td>89B PL 62 1825</td><td>F. Abe et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABE</td><td>89D PRL 63 1447</td><td>F. Abe et al.</td><td>(CDF Collab.)</td></tr><tr><td>ABE</td><td>89J ZPHY C45 175</td><td>K. Abe et al.</td><td>(VENUS Collab.)</td></tr><tr><td>ALBAJAR</td><td>89 ZPHY C44 15</td><td>K. Albajar et al.</td><td>(UA1 Collab.)</td></tr><tr><td>BARGER</td><td>89 PL B220 464</td><td>C. Barger et al.</td><td>(WISC, KEK)</td></tr><tr><td>DORENBOSS</td><td>89 ZPHY C41 567</td><td>J. Dorenbosch et al.</td><td>(CHARM Collab.)</td></tr><tr><td>BARTEL</td><td>87B ZPHY C36 15</td><td>W. Bartel et al.</td><td>(JADE Collab.)</td></tr><tr><td>GRIFOLS</td><td>86 PL 168B 264</td><td>J.A. Grifols, S. Peris</td><td>(BAR Collab.)</td></tr><tr><td>JODIDIO</td><td>86 A. Jodidio et al.</td><td>A. Jodidio et al.</td><td>(LBL, NWES, TRIU)</td></tr><tr><td>Also</td><td>PR D37 237 (errat.)</td><td>A. Jodidio et al.</td><td>(LBL, NWES, TRIU)</td></tr><tr><td>RENARD</td><td>82 PL 116B 264</td><td>F.M. Renard</td><td>(CERN)</td></tr></table>

### Extra Dimensions

For explanation of terms used and discussion of significant model dependence of following limits, see the "Extra Dimensions" review. Footnotes describe originally quoted limit. $\delta$ indicates the number of extra dimensions.

Limits not encoded here are summarized in the "Extra Dimensions" review, where the latest unpublished results are also described.

### See the related review(s):

#### Extra Dimensions

#### CONTENTS:

* Limits on $R$ from Deviations in Gravitational Force Law

* Limits on $R$ from On-Shell Production of Gravitons: $\delta = 2$

* Mass Limits on $M_{TT}$

* Limits on $1/R = M_c$

* Limits on Kaluza-Klein Gravitons in Warped Extra Dimensions

* Limits on Kaluza-Klein Gluons in Warped Extra Dimensions

* Black Hole Production Limits

- Semiclassical Black Holes

- Quantum Black Holes
## Limits on R from Deviations in Gravitational Force Law

This section includes limits on the size of extra dimensions from deviations in the Newtonian $(1/R^2)$ gravitational force law at short distances. Deviations are parametrized by a gravitational potential of the form $V = -(G m^2/r)$ [1 + $\alpha$ exp($-r/R$)]. For $\delta$ toroidal extra dimensions of equal size, $\alpha = 8\delta/3$. Quoted bounds are for $\delta = 2$ unless otherwise noted.

<table><thead><tr><th>VALUE (μm)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td rowspan="10">&lt; 37</td><td rowspan="10">95</td><td>1 BLAKEMORE</td><td>21</td><td>Optical levitation</td></tr><tr><td>2 HEACOCK</td><td>21</td><td>Neutron scattering</td></tr><tr><td>3 LEE</td><td>20</td><td>Torsion pendulum</td></tr><tr><td>4 TAN</td><td>20A</td><td>Torsion pendulum</td></tr><tr><td>5 BERGE</td><td>18</td><td>MICR</td><td>Space accelerometer</td></tr><tr><td>6 FAYET</td><td>18A</td><td>MICR</td><td>Space accelerometer</td></tr><tr><td>7 KLIMCHITSK...17A</td><td></td><td></td><td>Torsion oscillator</td></tr><tr><td>8 XU</td><td>13</td><td></td><td>Nuclei properties</td></tr><tr><td>9 BEZERRA</td><td>11</td><td></td><td>Torsion oscillator</td></tr><tr><td>10 SUSHKOV</td><td>11</td><td></td><td>Torsion pendulum</td></tr><tr><td>11 BEZERRA</td><td>10</td><td></td><td>Microcantilever</td></tr><tr><td>12 MASUDA</td><td>09</td><td></td><td>Torsion pendulum</td></tr><tr><td>13 GERACI</td><td>08</td><td></td><td>Microcantilever</td></tr><tr><td>14 TRENKEL</td><td>08</td><td></td><td>Newton's constant</td></tr><tr><td>15 DECCA</td><td>07A</td><td></td><td>Torsion oscillator</td></tr><tr><td rowspan="5">&lt; 37</td><td rowspan="5">95</td><td>16 KAPNER</td><td>07</td><td>Torsion pendulum</td></tr><tr><td>17 TU</td><td>07</td><td>Torsion pendulum</td></tr><tr><td>18 SMULLIN</td><td>05</td><td>Microcantilever</td></tr><tr><td>19 HOYLE</td><td>04</td><td>Torsion pendulum</td></tr><tr><td>20 CHIAVERINI</td><td>03</td><td>Microcantilever</td></tr><tr><td rowspan="2">&lt; 47</td><td rowspan="2">95</td><td>21 LONG</td><td>03</td><td>Microcantilever</td></tr><tr><td>22 HOYLE</td><td>01</td><td>Torsion pendulum</td></tr><tr><td>&lt;190</td><td>95</td><td>23 HOSKINS</td><td>85</td><td>Torsion pendulum</td></tr></tbody></table>

1. BLAKEMORE 21 obtain constraints on non-Newtonian forces with strengths $|\alpha| \gtrsim 10^8$ and length scales $R > 10$ µm. See their Fig. 4 for more details including comparison with previous searches.

2. HEACOCK 21 obtain constraints on non-Newtonian forces with strengths $10^{18} \lesssim |\alpha| \lesssim 10^{25}$ and length scales $R \approx 0.02-10$ nm. See their Figure 3 for more details. This improves the results of HADDOCK 18. These constraints do not place limits on the size of extra flat dimensions.

3. LEE 20 search for new forces probing a range of $|\alpha| \approx 0.1-10^5$ and length scales $R \approx 7-90$ µm. For $\delta = 1$ the bound on $R$ is 30 µm. See their Fig. 5 for details on the bound.

4. TAN 20A search for new forces probing a range of $|\alpha| \approx 4 \times 10^{-3}-1 \times 10^2$ and length scales $R \approx 40-350$ µm. See their Fig. 6 for details on the bound.

5. BERGE 18 uses results from the MICROSCOPE experiment to obtain constraints on non-Newtonian forces with strengths $10^{-11} \lesssim |\alpha| \lesssim 10^{-7}$ and length scales $R \gtrsim 10^5$ nm. See their Figure 1 for more details. These constraints do not place limits on the size of extra flat dimensions.

6. FAYET 18a uses results from the MICROSCOPE experiment to obtain constraints on an EP-violating force possibly arising from a new U(1) gauge boson. For $R \gtrsim 10^7$ m the limits are $|\alpha| \lesssim 10^{-4}$ a few $10^{-13}$ to a few $10^{-11}$ depending on the coupling, corresponding to $|\alpha| \lesssim 10^{-24}$ for the coupling of the new spin-1 or spin-0 mediator. These constraints do not place limits on the size of extra flat dimensions. This extends the results of FAYET 18.

7. KLIMCHITSKAYA 17A uses an experiment that measures the difference of Casimir forces to obtain bounds on non-Newtonian forces with strengths $|\alpha| \approx 10^{5}-10^{17}$ and length scales $R = 0.03-10$ µm. See their Fig. 3. These constraints do not place limits on the size of extra flat dimensions.

8. XU 13 obtain constraints on non-Newtonian forces with strengths $|\alpha| \approx 10^{34}-10^{36}$ and length scales $R \approx 1-10$ fm. See their Fig. 4 for more details. These constraints do not place limits on the size of extra flat dimensions.

9. BEZERRA 11 obtain constraints on non-Newtonian forces with strengths $10^{11} \lesssim |\alpha| \lesssim 10^{18}$ and length scales $R = 30-1260$ nm. See their Fig. 2 for more details. These constraints do not place limits on the size of extra flat dimensions.

10. SUSHKOV 11 obtain improved limits on non-Newtonian forces with strengths $10^7 \lesssim |\alpha| \lesssim 10^{11}$ and length scales $0.4$ µm $< R < 4$ µm (95% CL). See their Fig. 2. These bounds do not place limits on the size of extra flat dimensions. However, a model dependent bound of $M_\gamma > 70$ TeV is obtained assuming gauge bosons that couple to baryon number also propagate in $(4+\delta)$ dimensions.

11. BEZERRA 10 obtain improved constraints on non-Newtonian forces with strengths $10^{19} \lesssim |\alpha| \lesssim 10^{29}$ and length scales $R = 1.6-14$ nm (95% CL). See their Fig. 1. This bound does not place limits on the size of extra flat dimensions.

12. MASUDA 09 obtain improved constraints on non-Newtonian forces with strengths $10^9 \lesssim |\alpha| \lesssim 10^{11}$ and length scales $R = 1.0-2.9$ µm (95% CL). See their Fig. 3. This bound does not place limits on the size of extra flat dimensions.

13. GERACI 08 obtain improved constraints on non-Newtonian forces with strengths $|\alpha| > 14,000$ and length scales $R = 5-15$ µm. See their Fig. 9. This bound does not place limits on the size of extra flat dimensions.

14. TRENKEL 08 uses two independent measurements of Newton's constant $G$ to constrain new forces with strength $|\alpha| \approx 10^{-4}$ and length scales $R = 0.02-1$ m. See their Fig. 1. This bound does not place limits on the size of extra flat dimensions.

15. DECCA 07A search for new forces and obtain bounds in the region with strengths $|\alpha| \approx 10^{13}-10^{18}$ and length scales $R = 20-86$ nm. See their Fig. 6. This bound does not place limits on the size of extra flat dimensions.

16. KAPNER 07 search for new forces, probing a range of $|\alpha| \approx 10^{-3}-10^5$ and length scales $R \approx 10-1000$ µm. For $\delta = 1$ the bound on $R$ is 44 µm. For $\delta = 2$, the bound is expressed in terms of $M_\gamma$, here translated to a bound on the radius. See their Fig. 6 for details on the bound.

17. TU 07 search for new forces probing a range of $|\alpha| \approx 10^{-1}-10^5$ and length scales $R \approx 20-1000$ µm. For $\delta = 1$ the bound on $R$ is 53 µm. See their Fig. 3 for details on the bound.

18. SMULLIN 05 search for new forces, and obtain bounds in the region with strengths $\alpha \approx 10^3-10^8$ and length scales $R = 6-20$ µm. See their Figs. 1 and 16 for details on the bound. This work does not place limits on the size of extra flat dimensions.

19. HOYLE 04 search for new forces, probing $\alpha$ down to $10^{-2}$ and distances down to $10\mu m$. Quoted bound on $R$ is for $\delta = 2$. For $\delta = 1$, bound goes to $160$ µm. See their Fig. 34 for details on the bound.

20. CHIAVERINI 03 search for new forces, probing $\alpha$ above $10^4$ and $\lambda$ down to $3\mu m$, finding no signal. See their Fig. 4 for details on the bound. This bound does not place limits on the size of extra flat dimensions.

21. LONG 03 search for new forces, probing $\alpha$ down to 3, and distances down to about $10\mu m$. See their Fig. 4 for details on the bound.

22. HOYLE 01 search for new forces, probing $\alpha$ down to $10^{-2}$ and distances down to $20\mu m$. See their Fig. 4 for details on the bound. The quoted bound is for $\alpha \ge 3$.

23. HOSKINS 85 search for new forces, probing distances down to 4 mm. See their Fig. 13 for details on the bound. This bound does not place limits on the size of extra flat dimensions.

## Limits on R from On-Shell Production of Gravitons: $\delta = 2$

This section includes limits on on-shell production of gravitons in collider and astrophysical processes. Bounds quoted are on $R$, the assumed common radius of the flat extra dimensions, for $\delta = 2$ extra dimensions. Studies often quote bounds in terms of derived parameter; experiments are actually sensitive to the masses of the KK gravitons: $m_{\tilde{n}} = |\tilde{n}|/R$. See the Review on "Extra Dimensions" for details. Bounds are given in $\mu m$ for $\delta = 2$.

<table><thead><tr><th>VALUE (μm)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt; 3.8</td><td>95</td><td>1 AAD</td><td>21F</td><td>pp → jG</td></tr><tr><td>&lt; 0.00016</td><td>95</td><td>2 HANNESTAD</td><td>03</td><td>Neutron star heating</td></tr><tr><td>&lt; 56</td><td>95</td><td>3 SIRUNYAN</td><td>21A</td><td>CMS pp → ZG</td></tr><tr><td>&lt; 4.1</td><td>95</td><td>4 TUMASYAN</td><td>21D</td><td>CMS pp → jG</td></tr><tr><td>&lt; 90</td><td>95</td><td>5 SIRUNYAN</td><td>17AQ</td><td>CMS pp → γG</td></tr><tr><td>&lt; 127</td><td>95</td><td>6 AABOUD</td><td>16F</td><td>ATLS pp → γG</td></tr><tr><td>&lt; 34.4</td><td>95</td><td>8 AAD</td><td>15CS</td><td>ATLS pp → γG</td></tr><tr><td>&lt; 0.0087</td><td>95</td><td>10 AAD</td><td>13D</td><td>ATLS pp → jJ</td></tr><tr><td>&lt; 245</td><td>95</td><td>11 AJELLO</td><td>12</td><td>FLAT Neutron star γ sources</td></tr><tr><td>&lt; 615</td><td>95</td><td>12 AALTONEN</td><td>08AC</td><td>CDF p̄ → γG, jG</td></tr><tr><td>&lt; 0.916</td><td>95</td><td>13 ABAZOV</td><td>08S</td><td>D0 p̄ → γG</td></tr><tr><td>&lt; 350</td><td>95</td><td>14 DAS</td><td>08</td><td>Supernova cooling</td></tr><tr><td>&lt; 270</td><td>95</td><td>15 ABULENCIA,A</td><td>06</td><td>CDF p̄ → jG</td></tr><tr><td>&lt; 210</td><td>95</td><td>16 ABDALLAH</td><td>05B</td><td>DLPH e⁺ e⁻ → γG</td></tr><tr><td>&lt; 480</td><td>95</td><td>17 ACHARD</td><td>04E</td><td>L3 e⁺ e⁻ → γG</td></tr><tr><td>&lt; 0.00038</td><td>95</td><td>18 ACOSTA</td><td>04C</td><td>CDF p̄ → jG</td></tr><tr><td>&lt; 610</td><td>95</td><td>19 CASSE</td><td>04</td><td>Neutron star γ sources</td></tr><tr><td>&lt; 0.96</td><td>95</td><td>20 ABAZOV</td><td>03</td><td>D0 p̄ → jG</td></tr><tr><td>&lt; 0.096</td><td>95</td><td>21 HANNESTAD</td><td>03</td><td>Supernova cooling</td></tr><tr><td>&lt; 0.051</td><td>95</td><td>22 HANNESTAD</td><td>03</td><td>Diffuse γ background</td></tr><tr><td>&lt; 300</td><td>95</td><td>23 HANNESTAD</td><td>03</td><td>Neutron star γ sources</td></tr><tr><td>&lt; 0.66</td><td>95</td><td>24 HEISTER</td><td>03C</td><td>ALEC e⁺ e⁻ → γG</td></tr><tr><td>&lt;1300</td><td>95</td><td>25 FAIRBAIRN</td><td>01</td><td>Cosmology</td></tr><tr><td></td><td></td><td>26 HANHART</td><td>01</td><td>Supernova cooling</td></tr><tr><td></td><td></td><td>27 CASSISI</td><td>00</td><td>Red giants</td></tr><tr><td></td><td></td><td>28 ACCIARRI</td><td>99S</td><td>L3 e⁺ e⁻ → ZG</td></tr></tbody></table>

1. AAD 21F search for $pp \to jG$, using $139 \text{ fb}^{-1}$ of data at $\sqrt{s} = 13$ TeV to place lower limits on $M_D$ for two to six extra dimensions (see their Table X), from which this bound on $R$ is derived. This limit supersedes that in AABOUD 18.

2. HANNESTAD 03 obtain a limit on $R$ from the heating of old neutron stars by the surrounding cloud of trapped KK gravitons. Limits for all $\delta \le 7$ are given in their Tables V and VI. These limits supersedes those in HANNESTAD 02.

3. SIRUNYAN 21A search for $pp \to ZG$, using $137 \text{ fb}^{-1}$ of data at $\sqrt{s} = 13$ TeV to place lower limits on $M_D$ for two to seven extra dimensions (see their Figure 12), from which this bound on $R$ is derived. These limits supersedes those obtained in SIRUNYAN 18B.

4. TUMASYAN 21D search for $pp \to jG$, using $137 \text{ fb}^{-1}$ of data at $\sqrt{s} = 13$ TeV to place lower limits on $M_D$ for two to seven extra dimensions (see their Table 3), from which this bound on $R$ is derived. This limit supersedes that in SIRUNYAN 18S.

5. SIRUNYAN 17AQ search for $pp \to \gamma G$, using $12.9 \text{ fb}^{-1}$ of data at $\sqrt{s} = 13$ TeV to place limits on $M_D$ for three to six extra dimensions (see their Table 3).

6. AABOUD 16F search for $pp \to \gamma G$, using $3.2 \text{ fb}^{-1}$ of data at $\sqrt{s} = 13$ TeV to place limits on $M_D$ for two to six extra dimensions (see their Figure 9), from which this bound on $R$ is derived.

7. KHACHATRYAN 16N search for $pp \to \gamma G$, using $19.6 \text{ fb}^{-1}$ of data at $\sqrt{s} = 8$ TeV to place limits on $M_D$ for three to six extra dimensions (see their Table 5).

8. AAD 15CS search for $pp \to \gamma G$, using $20.3 \text{ fb}^{-1}$ of data at $\sqrt{s} = 8$ TeV to place lower limits on $M_D$ for two to six extra dimensions (see their Fig. 18).

9. AAD 13C search for $pp \to \gamma G$, using $4.6 \text{ fb}^{-1}$ of data at $\sqrt{s} = 7$ TeV to place bounds on $M_D$ for two to six extra dimensions, from which this bound on $R$ is derived.

10. AAD 13D search for the dijet decay of quantum black holes in $4.8 \text{ fb}^{-1}$ of data produced in $p\bar{p}$ collisions at $\sqrt{s} = 7$ TeV to place bounds on $M_D$ for two to seven extra dimensions, from which these bounds on $R$ are derived. Limits on $M_D$ for all $\delta \le 7$ are given in their Table 3.

11. AJELLO 12 obtain a limit on $R$ from the gamma-ray emission of point $\gamma$ sources that arise from the photon decay of KK gravitons which are gravitationally bound around neutron stars. Limits for all $\delta \le 7$ are given in their Table 7.

12. AALTONEN 08AC search for $p\bar{p} \to \gamma G$ and $p\bar{p} \to jG$ at $\sqrt{s} = 1.96$ TeV with $2.0 \text{ fb}^{-1}$ and $1.1 \text{ fb}^{-1}$ respectively, in order to place bounds on the fundamental scale and size of the extra dimensions. See their Table III for limits on all $\delta \le 6$.

13. ABAZOV 08S search for $p\bar{p} \to \gamma G$, using $1 \text{ fb}^{-1}$ of data at $\sqrt{s} = 1.96$ TeV to place bounds on $M_D$ for two to eight extra dimensions, from which these bounds on $R$ are derived. See their paper for intermediate values of $\delta$.
# Searches Particle Listings
## Extra Dimensions

¹⁴DAS 08 obtain a limit on R from Kaluza-Klein graviton cooling of SN1987A due to plasmon-plasmon annihilation.

¹⁵ABULENCIA, A 06 search for $p\bar{p} \to jG$ using 368 pb⁻¹ of data at $\sqrt{s} = 1.96$ TeV. See their Table II for bounds for all $\delta \le 6$.

¹⁶ABDALLAH 05b search for $e^+e^- \to \gamma G$ at $\sqrt{s} = 180-209$ GeV to place bounds on the size of extra dimensions and the fundamental scale. Limits for all $\delta \le 6$ are given in their Table 6. These limits supersede those in ABREU 002.

¹⁷ACHER 04e search for $e^+e^- \to \gamma G$ at $\sqrt{s} = 189-209$ GeV to place bounds on the size of extra dimensions and the fundamental scale. See their Table 8 for limits with $\delta \le 8$. These limits supersede those in ACCIARRI 99r.

¹⁸ACOSTA 04c search for $p\bar{p} \to jG$ at $\sqrt{s} = 1.8$ TeV to place bounds on the size of extra dimensions and the fundamental scale. See their paper for bounds on $\delta = 4, 6$.

¹⁹CASSE 04 obtain a limit on R from the gamma-ray emission of point $\gamma$ sources that arises from the photon decay of gravitons around newly born neutron stars, applying the technique of HANNESTAD 03 to neutron stars in the galactic bulge. Limits for all $\delta \le 7$ are given in their Table I.

²⁰ABAZOV 03 search for $p\bar{p} \to jG$ at $\sqrt{s}=1.8$ TeV to place bounds on $M_D$ for 2 to 7 extra dimensions, from which these bounds on R are derived. See their paper for bounds on intermediate values of $\delta$. We quote results without the approximate NLO scaling introduced in the paper.

²¹HANNESTAD 03 obtain a limit on R from graviton cooling of supernova SN1987a. Limits for all $\delta \le 7$ are given in their Tables V and VI.

²²HANNESTAD 03 obtain a limit on R from gravitons emitted in supernovae and which subsequently decay, contaminating the diffuse cosmic $\gamma$ background. Limits for all $\delta \le 7$ are given in their Tables V and VI. These limits supersede those in HANNESTAD 02.

²³HANNESTAD 03 obtain a limit on R from gravitons emitted in two recent supernovae and which subsequently decay, creating point $\gamma$ sources. Limits for all $\delta \le 7$ are given in their Tables V and VI. These limits are corrected in the published erratum.

²⁴HEISTER 03c use the process $e^+e^- \to \gamma G$ at $\sqrt{s} = 189-209$ GeV to place bounds on the size of extra dimensions and the scale of gravity. See their Table 4 for limits with $\delta \le 6$ for derived limits on $M_D$.

²⁵FAIRBAIRN 01 obtains bounds on R from over production of KK gravitons in the early universe. Bounds are quoted in paper in terms of fundamental scale of gravity. Bounds depend strongly on temperature of QCD phase transition and range from $R \sim 0.13$ µm to 0.001 µm for $\delta=2$; bounds for $\delta=3,4$ can be derived from Table 1 in the paper.

²⁶HANHART 01 obtain bounds on R from limits on graviton cooling of supernova SN 1987a using numerical simulations of proto-neutron star neutrino emission.

²⁷CASSISI 00 obtain rough bounds on $M_D$ (and thus R) from red giant cooling for $\delta=2,3$. See their paper for details.

²⁸ACCIARRI 99s search for $e^+e^- \to ZG$ at $\sqrt{s}=189$ GeV. Limits on the gravity scale are found in their Table 2, for $\delta \le 4$.

## Mass Limits on $M_{TT}$

This section includes limits on the cut-off mass scale, $M_{TT}$, of dimension-8 operators from KK graviton exchange in models of large extra dimensions. Ambiguities in the UV-divergent summation are absorbed into the parameter $\lambda$, which is taken to be $\lambda = \pm 1$ in the following analyses. Bounds for $\lambda = -1$ are shown in parenthesis after the bound for $\lambda = +1$, if appropriate. Different papers use slightly different definitions of the mass scale. The definition used here is related to another popular convention by $M_{TT}^2 = (2/\pi) \Lambda_T^4$, as discussed in the above Review on "Extra Dimensions."

<table><thead><tr><th>VALUE (TeV)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt; 9.02</td><td>95</td><td>1 SIRUNYAN</td><td>18DD CMS</td><td>p p → dijet, ang. distrib.</td></tr><tr><td>&gt;20.6</td><td>(&gt; 15.7)</td><td>2 GIUDICE</td><td>03 RVUE</td><td>Dim-6 operators</td></tr><tr><td colspan="5">● ● ● We do not use the following data for averages, fits, limits, etc. ● ● ●</td></tr><tr><td>&gt; 6.7</td><td>95</td><td>3 SIRUNYAN</td><td>21N CMS</td><td>p p → e<sup>+</sup>e<sup>-</sup>, μ<sup>+</sup>μ<sup>-</sup></td></tr><tr><td>&gt; 6.9</td><td>95</td><td>4 SIRUNYAN</td><td>19AC CMS</td><td>p p → e<sup>+</sup>e<sup>-</sup>, μ<sup>+</sup>μ<sup>-</sup>, γγ</td></tr><tr><td>&gt; 7.0</td><td>(&gt;5.6)</td><td>5 SIRUNYAN</td><td>18DU CMS</td><td>p p → γγ</td></tr><tr><td>&gt; 6.5</td><td>95</td><td>6 AABOUD</td><td>17AP ATLS</td><td>p p → γγ</td></tr><tr><td>&gt; 3.8</td><td>95</td><td>7 AAD</td><td>14BE ATLS</td><td>p p → e<sup>+</sup>e<sup>-</sup>, μ<sup>+</sup>μ<sup>-</sup></td></tr><tr><td>&gt; 3.2</td><td>95</td><td>8 AAD</td><td>13E ATLS</td><td>p p → e<sup>+</sup>e<sup>-</sup>, μ<sup>+</sup>μ<sup>-</sup>, γγ</td></tr><tr><td></td><td></td><td>9 BAAK</td><td>12 RVUE</td><td>Electroweak</td></tr><tr><td>&gt; 0.90</td><td>(&gt;0.92)</td><td>10 AARON</td><td>11C H1</td><td>e<sup>±</sup> p → e<sup>±</sup>X</td></tr><tr><td>&gt; 1.48</td><td>95</td><td>11 ABAZOV</td><td>09AE D0</td><td>p p → dijet, ang. distrib.</td></tr><tr><td>&gt; 1.45</td><td>95</td><td>12 ABAZOV</td><td>09D D0</td><td>p p → e<sup>+</sup>e<sup>-</sup>, γγ</td></tr><tr><td>&gt; 1.1</td><td>(&gt; 1.0)</td><td>13 SCHAEL</td><td>07A ALEP</td><td>e<sup>+</sup>e<sup>-</sup> → e<sup>+</sup>e<sup>-</sup></td></tr><tr><td>&gt; 0.898</td><td>(&gt; 0.998)</td><td>14 ABDALLAH</td><td>06C DLPH</td><td>e<sup>+</sup>e<sup>-</sup> → ℓ<sup>+</sup>ℓ<sup>-</sup></td></tr><tr><td>&gt; 0.853</td><td>(&gt; 0.939)</td><td>15 GERDES</td><td>06</td><td>p p → e<sup>+</sup>e<sup>-</sup>, γγ</td></tr><tr><td>&gt; 0.96</td><td>(&gt; 0.93)</td><td>16 ABAZOV</td><td>05V D0</td><td>p p → μ<sup>+</sup>μ<sup>-</sup></td></tr><tr><td>&gt; 0.78</td><td>(&gt; 0.79)</td><td>17 CHEKANOV</td><td>04B ZEUS</td><td>e<sup>±</sup> p → e<sup>±</sup>X</td></tr><tr><td>&gt; 0.805</td><td>(&gt; 0.956)</td><td>18 ABIENDI</td><td>03D OPAL</td><td>e<sup>+</sup>e<sup>-</sup> → γγ</td></tr><tr><td>&gt; 0.7</td><td>(&gt; 0.7)</td><td>19 ACHARD</td><td>03D L3</td><td>e<sup>+</sup>e<sup>-</sup> → ZZ</td></tr><tr><td>&gt; 0.82</td><td>(&gt; 0.78)</td><td>20 ADLOFF</td><td>03 H1</td><td>e<sup>±</sup> p → e<sup>±</sup>X</td></tr><tr><td>&gt; 1.28</td><td>(&gt; 1.25)</td><td>21 GIUDICE</td><td>03 RVUE</td><td></td></tr><tr><td>&gt; 0.80</td><td>(&gt; 0.85)</td><td>22 HEISTER</td><td>03C ALEP</td><td>e<sup>+</sup>e<sup>-</sup> → γγ</td></tr><tr><td>&gt; 0.84</td><td>(&gt; 0.99)</td><td>23 ACHARD</td><td>02D L3</td><td>e<sup>+</sup>e<sup>-</sup> → γγ</td></tr><tr><td>&gt; 1.2</td><td>(&gt; 1.1)</td><td>24 ABBOTT</td><td>01 D0</td><td>p p → e<sup>+</sup>e<sup>-</sup>, γγ</td></tr><tr><td>&gt; 0.60</td><td>(&gt; 0.63)</td><td>25 ABIENDI</td><td>00R OPAL</td><td>e<sup>+</sup>e<sup>-</sup> → μ<sup>+</sup>μ<sup>-</sup></td></tr><tr><td>&gt; 0.63</td><td>(&gt; 0.50)</td><td>25 ABIENDI</td><td>00R OPAL</td><td>e<sup>+</sup>e<sup>-</sup> → τ<sup>+</sup>τ<sup>-</sup></td></tr><tr><td>&gt; 0.68</td><td>(&gt; 0.61)</td><td>25 ABIENDI</td><td>00R OPAL</td><td>e<sup>+</sup>e<sup>-</sup> → μ<sup>+</sup>μ<sup>-</sup>, τ<sup>+</sup>τ<sup>-</sup></td></tr><tr><td></td><td></td><td>26 ABREU</td><td>00A DLPH</td><td>e<sup>+</sup>e<sup>-</sup> → γγ</td></tr><tr><td>&gt; 0.680</td><td>(&gt; 0.542)</td><td>27 ABREU</td><td>00S DLPH</td><td>e<sup>+</sup>e<sup>-</sup> → μ<sup>+</sup>μ<sup>-</sup>, τ<sup>+</sup>τ<sup>-</sup></td></tr><tr><td>&gt; 15-28</td><td>99.7</td><td>28 CHANG</td><td>00 RVUE</td><td>Electroweak</td></tr><tr><td>&gt; 0.98</td><td>95</td><td>29 CHEUNG</td><td>00 RVUE</td><td>e<sup>+</sup>e<sup>-</sup> → γγ</td></tr><tr><td>&gt; 0.29-0.38</td><td>95</td><td>30 GRAESSER</td><td>00 RVUE</td><td>(g-2)μ</td></tr><tr><td>&gt; 0.50-1.1</td><td>95</td><td>31 HAN</td><td>00 RVUE</td><td>Electroweak</td></tr><tr><td>&gt; 2.0</td><td>(&gt; 2.0)</td><td>32 MATHEWS</td><td>00 RVUE</td><td>p p → jj</td></tr></tbody></table>

1. $> 1.0$ ($> 1.1$) 95 $^{33}$MELE 00 RVUE $e^+e^- \to VV$

2. $> 34$ ABIENDI 99P OPAL

3. $> 35$ ACCIARRI 99M L3

4. $> 36$ ACCIARRI 99S L3

5. $> 1.412$ ($> 1.077$) 95 $^{37}$BOURILKOV 99 $e^+e^- \to e^+e^-$

1. SIRUNYAN 18DD use dijet angular distributions in 35.9 fb⁻¹ of data from $p p$ collisions at $\sqrt{s} = 13$ TeV to place a lower bound on $\Lambda_T$, here converted to $M_{TT}$. This updates the results of SIRUNYAN 17F.

2. GIUDICE 03 place bounds on $\Lambda_6$, the coefficient of the gravitationally-induced dimension-6 operator $(2\pi\lambda/\Lambda_6^2)(\sum T_\gamma\mu_\gamma\gamma^5)\sum T_\gamma\mu_\gamma\gamma^5)$, using data from a variety of experiments. Results are quoted for $\lambda = \pm 1$ and are independent of $\delta$.

3. SIRUNYAN 21N use 137 (140) fb⁻¹ of data from $p p$ collisions at $\sqrt{s} = 13$ TeV in the dielectron (dimuon) channels to place a lower limit on $\Lambda_T$, here converted to $M_{TT}$. Bounds on individual channels can be found in their Table 7.

4. SIRUNYAN 19AC use 35.9 (36.3) fb⁻¹ of data from $p p$ collisions at $\sqrt{s} = 13$ TeV in the dielectron (dimuon) channels to place a lower limit on $\Lambda_T$, here converted to $M_{TT}$. The dielectron and dimuon channels are combined with previous results in the diphoton channel to set the best limit. Bounds on individual channels and different priors can be found in their Table 2. This updates the results in KHACHATRYAN 15AE.

5. SIRUNYAN 18DU use 35.9 fb⁻¹ of data from $p p$ collisions at $\sqrt{s} = 13$ TeV to place lower limits on $M_{TT}$ (equivalent to their $M_S$). This updates the results of CHATRCHYAN 12R.

6. AABOUD 17AP use 36.7 fb⁻¹ of data from $p p$ collisions at $\sqrt{s} = 13$ TeV to place lower limits on $M_{TT}$ (equivalent to their $M_S$). This updates the results of AAD 13AS.

7. AAD 14BE use 20 fb⁻¹ of data from $p p$ collisions at $\sqrt{s} = 8$ TeV in the dilepton channel to place lower limits on $M_{TT}$ (equivalent to their $M_S$).

8. AAD 13E use 4.9 and 5.0 fb⁻¹ of data from $p p$ collisions at $\sqrt{s} = 7$ TeV in the dielectron and dimuon channels, respectively, to place lower limits on $M_{TT}$ (equivalent to their $M_S$). The dielectron and dimuon channels are combined with previous results in the diphoton channel to set the best limit. Bounds on individual channels and different priors can be found in their Table VIII.

9. BAAK 12 use electroweak precision observables to place bounds on the ratio $\Lambda_T/M_D$ as a function of $M_D$. See their Fig. 22 for constraints with a Higgs mass of 120 GeV.

10. AARON 11C search for deviations in the differential cross section of $e^{\pm} p \to e^{\pm} X$ in 446 fb⁻¹ of data taken at $\sqrt{s} = 301$ and 319 GeV to place a bound on $M_{TT}$.

11. ABAZOV 09AE use dijet angular distributions in 0.7 fb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to place lower bounds on $\Lambda_T$ (equivalent to their $M_S$), here converted to $M_{TT}$.

12. ABAZOV 09D use 1.05 fb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to place lower bounds on $\Lambda_T$ (equivalent to their $M_S$), here converted to $M_{TT}$.

13. SCHAEL 07A use $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV to place lower limits on $\Lambda_T$, here converted to limits on $M_{TT}$.

14. ABDALLAH 06C use $e^+e^-$ collisions at $\sqrt{s} \sim 130-207$ GeV to place lower limits on $M_{TT}$, which is equivalent to their definition of $M_S$. Bound shown includes all possible final state leptons, $\ell^-, e^+, \mu^-, \tau^-$, Bounds on individual leptonic final states can be found in their Table 31.

15. GERDES 06 use 100 to 110 pb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s} = 1.8$ TeV, as recorded by the CDF Collaboration during Run I of the Tevatron. Bound shown includes a K-factor of 1.3. Bounds on individual $e^+e^-$ and $\gamma\gamma$ final states are found in their Table I.

16. ABAZOV 05V use 246 pb⁻¹ of data from $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV to search for deviations in the differential cross section to $\mu^+\mu^-$ from graviton exchange.

17. CHEKANOV 04B search for deviations in the differential cross section of $e^{\pm} p \to e^{\pm} X$ with 130 pb⁻¹ of combined data and $Q^2$ values up to 40,000 GeV² to place a bound on $M_{TT}$.

18. ABIENDI 03D use $e^+e^-$ collisions at $\sqrt{s}=181-209$ GeV to place bounds on the ultraviolet scale $M_{TT}$, which is equivalent to their definition of $M_S$.

19. ACHARD 03D look for deviations in the cross section for $e^+e^- \to ZZ$ from $\sqrt{s} = 200-209$ GeV to place a bound on $M_{TT}$.

20. ADLOFF 03 search for deviations in the differential cross section of $e^{\pm} p \to e^{\pm} X$ at $\sqrt{s}=301$ and 319 GeV to place bounds on $M_{TT}$.

21. GIUDICE 01 review existing experimental bounds on $M_{TT}$ and derive a combined limit.

22. HEISTER 03c use $e^+e^-$ collisions at $\sqrt{s} = 189-209$ GeV to place bounds on the scale of dim-8 gravitational interactions. Their $M_S^\pm$ is equivalent to our $M_{TT}$ with $\lambda = \pm 1$.

23. ACHARD 02 search for s-channel graviton exchange effects in $e^+e^- \to \gamma\gamma$ at $E_{cm} = 192-209$ GeV.

24. ABBOTT 01 search for variations in differential cross sections to $e^+e^-$ and $\gamma\gamma$ final states at the Tevatron.

25. ABIENDI 00R uses $e^+e^-$ collisions at $\sqrt{s} = 189$ GeV.

26. ABREU 00A search for s-channel graviton exchange effects in $e^+e^- \to \gamma\gamma$ at $E_{cm} = 189-202$ GeV.

27. ABREU 00s uses $e^+e^-$ collisions at $\sqrt{s}=183$ and 189 GeV. Bounds on $\mu$ and $\tau$ individual final states given in paper.

28. CHANG 00b derive $3\sigma$ limit on $M_{TT}$ of (28,19,15) TeV for $\delta=(2,4,6)$ respectively assuming the presence of a torsional coupling in the gravitational action. Highly model dependent.

29. CHEUNG 00 obtains limits from anomalous diphoton production at OPAL due to graviton exchange. Original limit for $\delta=4$. However, unknown UV theory renders $\delta$ dependence unreliable. Original paper works in HLZ convention.

30. GRAESSER 00 obtains a bound from graviton contributions to $g-2$ of the muon through loops of 0.29 TeV for $\delta=2$ and 0.38 TeV for $\delta=4,6$. Limits scale as $\lambda^{1/2}$. However calculational scheme not well-defined without specification of high-scale theory. See the "Extra Dimensions Review."

31. HAN 00 calculates corrections to gauge boson self-energies from KK graviton loops and constrain them using $S$ and $T$. Bounds on $M_{TT}$ range from 0.5 TeV ($\delta=6$) to 1.1 TeV ($\delta=2$); see text. Limits have strong dependence, $\lambda^{\delta+2}$, on unknown $\lambda$ coefficient.

32. MATHEWS 00 search for evidence of graviton exchange in CDF and DØ dijet production data. See their Table 2 for slightly stronger $\delta$-dependent bounds. Limits expressed in terms of $M_S^4 = M_{TT}^4/8$.

33. MELE 00 obtains bound from KK graviton contributions to $e^+e^- \to VV$ ($V=\gamma, W, Z$) at LEP. Authors use Hewett conventions.