| $\bf{
1.36 \pm0.17}$
|
OUR AVERAGE
|
| $0.0$ ${}^{+1.3}_{-0.4}$ |
|
1 |
|
NOVA |
| $1.33$ ${}^{+0.45}_{-0.51}$ |
|
2 |
|
SKAM |
| $1.40$ $\pm0.20$ |
|
3 |
|
T2K |
| • • • We do not use the following data for averages, fits, limits, etc. • • • |
| $1.33$ ${}^{+0.46}_{-0.53}$ |
|
4 |
|
SKAM |
| $1.22$ ${}^{+0.76}_{-0.67}$ |
|
4 |
|
SKAM |
| $1.33$ ${}^{+0.48}_{-0.53}$ |
|
2 |
|
SKAM |
| $1.54$ ${}^{+0.14}_{-0.12}$ |
95 |
3 |
|
T2K |
| $1.21$ ${}^{+0.91}_{-0.30}$ |
|
5 |
|
NOVA |
| $1.46$ ${}^{+0.56}_{-0.42}$ |
|
5 |
|
NOVA |
| $1.32$ ${}^{+0.21}_{-0.15}$ |
|
|
|
FIT |
| $1.56$ ${}^{+0.13}_{-0.15}$ |
|
|
|
FIT |
| $1.45$ ${}^{+0.27}_{-0.26}$ |
|
6 |
|
T2K |
| $1.54$ ${}^{+0.22}_{-0.23}$ |
|
6 |
|
T2K |
| $1.50$ ${}^{+0.53}_{-0.57}$ |
|
7 |
|
NOVA |
| $0.74$ ${}^{+0.57}_{-0.93}$ |
|
7 |
|
NOVA |
| $1.48$ ${}^{+0.69}_{-0.58}$ |
|
7 |
|
NOVA |
| $\text{ 0.0 to 0.1, 0.5 to 2.0}$ |
90 |
8, 7 |
|
NOVA |
| $0.0\text{ to }2.0 $ |
90 |
8 |
|
NOVA |
| $\text{ 0 to 0.15, 0.83 to 2}$ |
90 |
|
|
T2K |
| $1.09\text{ to }1.92 $ |
90 |
|
|
T2K |
| $0.05\text{ to }1.2 $ |
90 |
9 |
|
MINS |
| $1.34$ ${}^{+0.64}_{-0.38}$ |
|
|
|
FIT |
| $1.48$ ${}^{+0.34}_{-0.32}$ |
|
|
|
FIT |
| $1.70$ ${}^{+0.22}_{-0.39}$ |
|
10 |
|
FIT |
| $1.41$ ${}^{+0.35}_{-0.34}$ |
|
10 |
|
FIT |
| $\text{ 0 to 1.5 or 1.9 to 2}$ |
90 |
11 |
|
MINS |
|
1
ACERO 2019 is based on a sample size of $1.33 \times 10^{20}$ protons on target with combined antineutrino and neutrino data. Supersedes ACERO 2018 .
|
|
2
ABE 2018B uses 328 kton$\cdot{}$years of Super-Kamiokande I-IV atmospheric neutrino data to obtain this result. The fit is performed over the three parameters, $\Delta $m${}^{2}_{32}$, sin$^2{{\mathit \theta}_{{23}}}$, and $\delta $, while the solar parameters and sin$^2{{\mathit \theta}_{{23}}}$ are fixed to $\Delta $m${}^{2}_{21}$= ($7.53$ $\pm0.18$) $ \times 10^{-5}$ eV${}^{2}$, sin$^2{{\mathit \theta}_{{12}}}$ = $0.304$ $\pm0.014$, and sin$^2{{\mathit \theta}_{{13}}}$ = $0.0219$ $\pm0.0012$.
|
|
3
ABE 2018G confidence intervals are marginalized over both mass orderings. Normal order preferred with a posterior probability of 87$\%$. The 1-sigma result for normal mass ordering used in the average was provided by the experiment via private communications. Supersedes ABE 2017F.
|
|
4
ABE 2018B uses 328 kton$\cdot{}$years of Super-Kamiokande I-IV atmospheric neutrino data to obtain this result. The fit is performed over the four parameters, $\Delta $m${}^{2}_{32}$, sin$^2{{\mathit \theta}_{{23}}}$, sin$^2{{\mathit \theta}_{{13}}}$, and $\delta $, while the solar parameters are fixed to $\Delta $m${}^{2}_{21}$= ($7.53$ $\pm0.18$) $ \times 10^{-5}$ eV${}^{2}$ and sin$^2{{\mathit \theta}_{{12}}}$ = $0.304$ $\pm0.014$.
|
|
5
ACERO 2018 performs a joint fit to the data for ${{\mathit \nu}_{{\mu}}}$ disappearance and ${{\mathit \nu}_{{e}}}$ appearance. The overall best fit favors normal mass ordering and ${{\mathit \theta}_{{23}}}$ in octant II. No 1$\sigma $ confidence intervals are presented for the inverted mass ordering scenarios. Superseded by ACERO 2019 .
|
|
6
ABE 2017F confidence intervals are obtained using a frequentist analysis including ${{\mathit \theta}_{{13}}}$ constraint from reactor experiments. Bayesian intervals based on Markov Chain Monte Carlo method are also provided by the authors. Superseded by ABE 2018G.
|
|
7
Errors are projections of 68$\%$ C.L. curve of $\delta _{CP}$ vs. sin$^2{{\mathit \theta}_{{23}}}$.
|
|
8
ADAMSON 2016 result is based on a data sample with $2.74 \times 10^{20}$ protons on target. The likelihood-based analysis observed 6 ${{\mathit \nu}_{{e}}}$ events with an expected background of $0.99$ $\pm0.11$ events.
|
|
9
ADAMSON 2014 result is based on three-flavor formalism and ${{\mathit \theta}_{{23}}}>{{\mathit \pi}}$/4. Likelihood as a function of $\delta $ is also shown for the other three combinations of hierarchy and ${{\mathit \theta}_{{23}}}$ octants; all values of $\delta $ are allowed at 90$\%$ C.L.
|
|
10
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as 68$\%$ CL intervals of $1.24 - 1.94$ for normal and $1.15 - 1.77$ for inverted mass ordering.
|
|
11
ADAMSON 2013A result is based on ${{\mathit \nu}_{{e}}}$ appearance in MINOS and the calculated sin$^2(2{{\mathit \theta}_{{23}}})$ = 0.957,${{\mathit \theta}_{{23}}}>{{\mathit \pi}}$/4, and normal mass hierarchy. Likelihood as a function of$\delta $ is also shown for the other three combinations of hierarchy and ${{\mathit \theta}_{{23}}}$ octants; all values of $\delta $ are allowed at 90$\%$ C.L.
|
