• • • We do not use the following data for averages, fits, limits, etc. • • • |
$<5$ |
90 |
1 |
|
MBNE |
$<7.2$ |
90 |
|
|
OPER |
$0.8\text{ to }3 $ |
90 |
2 |
|
MBNE |
$<11$ |
90 |
3 |
|
ICAR |
$<6.8$ |
90 |
4 |
|
ICAR |
$<100$ |
90 |
5 |
|
MBNE |
$<1.8$ |
90 |
6 |
|
MBNE |
$<110$ |
90 |
7 |
|
K2K |
$<1.4$ |
90 |
|
|
NOMD |
$<1.6$ |
90 |
|
|
NTEV |
|
|
8 |
|
LSND |
$0.5\text{ to }30 $ |
95 |
9 |
|
LSND |
$<3.0$ |
90 |
10 |
|
|
$<9.4$ |
90 |
|
|
CHM2 |
$<5.6$ |
90 |
11 |
|
CHM2 |
1
AGUILAR-AREVALO 2018C result is based on ${{\mathit \nu}_{{\mu}}}$ $\rightarrow$ ${{\mathit \nu}_{{e}}}$ appearance of $460.5$ $\pm99.0$ events; The best fit value is sin$^2(2\theta )$ = 0.92. The quoted limit for the two-neutrino mixing angle $\theta $ is valid above $\Delta $m${}^{2}$ = 0.59 eV${}^{2}$.
|
2
AGUILAR-AREVALO 2013A result is based on ${{\mathit \nu}_{{\mu}}}$ $\rightarrow$ ${{\mathit \nu}_{{e}}}$ appearance of $162.0$ $\pm47.8$ events; marginally compatible with two neutrino oscillations. The best fit value is sin$^2(2\theta )$ = 0.002.
|
3
ANTONELLO 2013 use the ICARUS T600 detector at LNGS and $\sim{}$20 GeV beam of ${{\mathit \nu}_{{\mu}}}$ from CERN 730 km away to search for an excess of ${{\mathit \nu}_{{e}}}$ events. Two events are found with $3.7$ $\pm0.6$ expected from conventional sources. This result excludes some parts of the parameter space expected by LSND. Superseded by ANTONELLO 2013A.
|
4
Based on four events with a background of $6.4$ $\pm0.9$ from conventional sources with an average energy of 20 GeV and 730 km from the source of ${{\mathit \nu}_{{\mu}}}$.
|
5
MAHN 2012 is a combined fit of MiniBooNE and SciBooNE neutrino data.
|
6
The limit is sin$^22\theta $ $<$ $0.9 \times 10^{-3}$ at $\Delta $ = 2 eV${}^{2}$. That value of $\Delta $ corresponds to the smallest mixing angle consistent with the reported signal from LSND in AGUILAR 2001 .
|
7
The limit becomes sin$^22\theta $ $<$ 0.15 at $\Delta $ = $2.8 \times 10^{-3}$ eV${}^{2}$, the bets-fit value of the ${{\mathit \nu}_{{\mu}}}$ disappearance analysis in K2K.
|
8
AGUILAR 2001 is the final analysis of the LSND full data set of the search for the ${{\mathit \nu}_{{\mu}}}$ $\rightarrow$ ${{\mathit \nu}_{{e}}}$ oscillations. See footnote in preceding table for further details.
|
9
ATHANASSOPOULOS 1998 report ($0.26$ $\pm0.10$ $\pm0.05)\%$ for the oscillation probability; the value of sin$^22\theta $ for large $\Delta \mathit m{}^{2}$ is deduced from this probability. See footnote in preceding table for further details, and see the paper for a plot showing allowed regions. If effect is due to oscillation, it is most likely to be intermediate sin$^22\theta $ and $\Delta \mathit m{}^{2}$. See also ATHANASSOPOULOS 1998B.
|
10
LOVERRE 1996 uses the charged-current to neutral-current ratio from the combined CHARM (ALLABY 1986 ) and CDHS (ABRAMOWICZ 1986 ) data from 1986.
|
11
VILAIN 1994C limit derived by combining the ${{\mathit \nu}_{{\mu}}}$ and ${{\overline{\mathit \nu}}_{{\mu}}}$ data assuming $\mathit CP$ conservation.
|