| • • • We do not use the following data for averages, fits, limits, etc. • • • |
|
|
|
1 |
|
MAJD |
| $<1 \times 10^{-8}$ |
90 |
0 |
2 |
|
CDM2 |
| $\sim$$6 \times 10^{-9}$ |
|
2 |
3 |
|
|
| $<1.4 \times 10^{-12}$ |
90 |
0 |
4 |
|
CALO |
|
|
|
5 |
|
PLAS |
| $<1.7 \times 10^{-11}$ |
99 |
0 |
6 |
|
CC |
| $<1. \times 10^{-9}$ |
90 |
0 |
7 |
|
CNTR |
| $2. \times 10^{-9}$ |
|
3 |
8 |
|
SPRK |
|
|
3 |
8 |
|
SPRK |
| $3.0 \times 10^{-9}$ |
|
3 |
9 |
|
SPRK |
| ($4$ $\pm1$) $ \times 10^{-11}$ |
|
3 |
|
|
ELEC |
| $<1.3 \times 10^{-9}$ |
90 |
|
10 |
|
CNTR |
| $<1.0 \times 10^{-9}$ |
|
0 |
|
|
ELEC |
| $<7. \times 10^{-10}$ |
90 |
0 |
|
|
ELEC |
| $>6. \times 10^{-9}$ |
|
5 |
11 |
|
CNTR |
| $<3.0 \times 10^{-8}$ |
|
0 |
|
|
CNTR |
| $<1.5 \times 10^{-9}$ |
|
0 |
|
|
CNTR |
| $<3.0 \times 10^{-10}$ |
|
0 |
|
|
CNTR |
| $<5.0 \times 10^{-11}$ |
90 |
0 |
|
|
ELEC |
|
1
ALVIS 2018 search for fractional charged flux of cosmic matter at Majorana demonstrator; no signal observed and limits are set on the flux of lightly ionizing particles for charge as low as e/1000.
|
|
2
See AGNESE 2015 Fig. 6 for limits extending down to Q = 1/200.
|
|
3
SAITO 1990 candidates carry about 450 MeV/nucleon. Cannot be accounted for by conventional backgrounds. Consistent with strange quark matter hypothesis.
|
|
4
MINCER 1985 is high statistics study of calorimeter signals delayed by 20$-$200 ns. Calibration with AGS beam shows they can be accounted for by rare fluctuations in signals from low-energy hadrons in the shower. Claim that previous delayed signals including BJORNBOE 1968 , DARDO 1972 , BHAT 1982 , SAKUYAMA 1983B below may be due to this fake effect.
|
|
5
SAKUYAMA 1983B analyzed 6000 extended air shower events. Increase of delayed particles and change of lateral distribution above $10^{17}$ eV may indicate production of very heavy parent at top of atmosphere.
|
|
6
BHAT 1982 observed 12 events with delay $>2. \times 10^{-8}~$s and with more than 40 particles. 1 eV has good hadron shower. However all events are delayed in only one of two detectors in cloud chamber, and could not be due to strongly interacting massive particle.
|
|
7
MARINI 1982 applied PEP-counter for TOF. Above limit is for velocity = 0.54 of light. Limit is inconsistent with YOCK 1980 YOCK 1981 events if isotropic dependence on zenith angle is assumed.
|
|
8
YOCK 1981 saw another 3 events with $\mathit Q$ = $\pm1$ and $\mathit m$ about 4.5${\mathit m}_{{{\mathit p}}}$ as well as 2 events with $\mathit m$ $>5.3{\mathit m}_{{{\mathit p}}}$, $\mathit Q$ = $\pm0.75\pm0.05$ and $\mathit m$ $>2.8{\mathit m}_{{{\mathit p}}}$, $\mathit Q$ = $\pm0.70\pm0.05$ and 1 event with $\mathit m$ = ($9.3$ $\pm3.){\mathit m}_{{{\mathit p}}}$, $\mathit Q$ = $\pm0.89\pm0.06$ as possible heavy candidates.
|
|
9
YOCK 1980 events are with charge exactly or approximately equal to unity.
|
|
10
BHAT 1978 is at Kolar gold fields. Limit is for $\tau $ $>10^{-6}$ s.
|
|
11
YOCK 1974 events could be tritons.
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