$0.307$ ${}^{+0.013}_{-0.012}$ |
1 |
|
FIT |
• • • We do not use the following data for averages, fits, limits, etc. • • • |
$0.320$ ${}^{+0.020}_{-0.016}$ |
|
|
FIT |
$0.310$ $\pm0.014$ |
2 |
|
FIT |
$0.334$ ${}^{+0.027}_{-0.023}$ |
3 |
|
FIT |
$0.327$ ${}^{+0.026}_{-0.031}$ |
4 |
|
FIT |
$0.323$ $\pm0.016$ |
5 |
|
FIT |
$0.304$ ${}^{+0.013}_{-0.012}$ |
6 |
|
FIT |
$0.299$ ${}^{+0.014}_{-0.014}$ |
7, 8 |
|
FIT |
$0.307$ ${}^{+0.016}_{-0.013}$ |
9, 8 |
|
FIT |
$0.304$ ${}^{+0.022}_{-0.018}$ |
10, 8 |
|
FIT |
$0.304$ ${}^{+0.014}_{-0.013}$ |
11 |
|
FIT |
$0.304$ ${}^{+0.014}_{-0.013}$ |
12 |
|
FIT |
$0.325$ ${}^{+0.039}_{-0.039}$ |
13 |
|
FIT |
$0.30$ ${}^{+0.02}_{-0.01}$ |
14 |
|
FIT |
$0.30$ ${}^{+0.02}_{-0.01}$ |
15 |
|
FIT |
$0.31$ ${}^{+0.03}_{-0.02}$ |
16 |
|
FIT |
$0.31$ ${}^{+0.03}_{-0.03}$ |
17 |
|
FIT |
$0.314$ ${}^{+0.015}_{-0.012}$ |
18 |
|
FIT |
$0.319$ ${}^{+0.017}_{-0.015}$ |
19 |
|
FIT |
$0.311$ ${}^{+0.016}_{-0.016}$ |
20 |
|
FIT |
$0.304$ ${}^{+0.046}_{-0.042}$ |
21 |
|
FIT |
$0.314$ ${}^{+0.018}_{-0.014}$ |
22, 23 |
|
FIT |
$0.314$ ${}^{+0.017}_{-0.020}$ |
22, 24 |
|
FIT |
$0.319$ ${}^{+0.019}_{-0.016}$ |
22, 25 |
|
FIT |
$0.319$ ${}^{+0.023}_{-0.024}$ |
22, 26 |
|
FIT |
$0.36$ ${}^{+0.05}_{-0.04}$ |
27 |
|
FIT |
$0.32$ $\pm0.03$ |
28 |
|
FIT |
$0.32$ $\pm0.02$ |
29 |
|
FIT |
$0.31$ ${}^{+0.04}_{-0.04}$ |
30 |
|
FIT |
$0.31$ ${}^{+0.04}_{-0.03}$ |
31 |
|
FIT |
$0.31$ ${}^{+0.03}_{-0.04}$ |
32 |
|
FIT |
$0.31$ ${}^{+0.02}_{-0.03}$ |
33 |
|
FIT |
$\text{0.25 - 0.39}$ |
34 |
|
FIT |
$0.29$ $\pm0.03$ |
35 |
|
FIT |
$0.29$ ${}^{+0.03}_{-0.02}$ |
36 |
|
FIT |
$\text{0.23 - 0.37}$ |
37 |
|
FIT |
$0.31$ ${}^{+0.04}_{-0.04}$ |
38 |
|
FIT |
$0.29$ ${}^{+0.04}_{-0.04}$ |
39 |
|
FIT |
$0.32$ ${}^{+0.06}_{-0.05}$ |
40 |
|
FIT |
$\text{0.19 - 0.33}$ |
41 |
|
FIT |
$\text{0.19 - 0.39}$ |
42 |
|
FIT |
1
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, using all solar data and KamLAND data. $\mathit CPT$ invariance is assumed.
|
2
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, using Super-Kamiokande (I+II+III+IV) and SNO data.
|
3
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, by combining the four phases of the Super-Kamiokande solar data.
|
4
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, using the Super-Kamiokande-IV data.
|
5
FORERO 2014 performs a global fit to neutrino oscillations using solar, reactor, long-baseline accelerator, and atmospheric neutrino data.
|
6
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 $0.304$ ${}^{+0.013}_{-0.012}$ for normal and $0.305$ ${}^{+0.012}_{-0.013}$ for inverted mass ordering.
|
7
AHARMIM 2013 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data.
|
8
AHARMIM 2013 global solar neutrino data include SNO's all-phases-combined analysis results on the total active ${}^{8}\mathrm {B}$ neutrino flux and energy-dependent ${{\mathit \nu}_{{e}}}$ survival probability parameters, measurements of ${}^{}\mathrm {Cl}$ (CLEVELAND 1998 ), ${}^{}\mathrm {Ga}$ (ABDURASHITOV 2009 which contains combined analysis with GNO (ALTMANN 2005 and Ph.D. thesis of F. Kaether)), and ${}^{7}\mathrm {Be}$ (BELLINI 2011A) rates, and ${}^{8}\mathrm {B}$ solar-neutrino recoil electron measurements of SK-I (HOSAKA 2006 ) zenith, SK-II (CRAVENS 2008 ) and SK-III (ABE 2011 ) day/night spectra, and Borexino (BELLINI 2010A) spectra.
|
9
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {32}}$ fixed to $2.45 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino data.
|
10
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {32}}$ fixed to $2.45 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino and KamLAND (GANDO 2011 ) data. CPT invariance is assumed.
|
11
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND, global solar neutrino, short-baseline (SBL) reactor, and accelerator data, assuming $\mathit CPT$ invariance. Supersedes GANDO 2011 .
|
12
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND and global solar neutrino data, assuming CPT invariance. Supersedes GANDO 2011 .
|
13
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND data. Supersedes GANDO 2011 .
|
14
ABE 2011 obtained this result by a two-neutrino oscillation analysis using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, SAGE, and KamLAND data. CPT invariance is assumed.
|
15
ABE 2011 obtained this result by a two-neutrino oscillation analysis using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, and SAGE data.
|
16
ABE 2011 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {32}}$ fixed to $2.4 \times 10^{-3}$ eV${}^{2}$, using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, SAGE, and KamLAND data. The normal neutrino mass ordering and CPT invariance are assumed.
|
17
ABE 2011 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {32}}$ fixed to $2.4 \times 10^{-3}$ eV${}^{2}$, using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, and GALLEX/GNO data. The normal neutrino mass ordering is assumed.
|
18
BELLINI 2011A obtained this result by a two-neutrino oscillation analysis using KamLAND, Homestake, SAGE, Gallex, GNO, Kamiokande, Super-Kamiokande, SNO, and Borexino (BELLINI 2011A) data and the SSM flux prediction in SERENELLI 2011 (Astrophysical Journal 743 24 (2011)) with the exception that the ${}^{8}\mathrm {B}$ flux was left free. CPT invariance is assumed.
|
19
BELLINI 2011A obtained this result by a two-neutrino oscillation analysis using Homestake, SAGE, Gallex, GNO, Kamiokande, Super-Kamiokande, SNO, and Borexino (BELLINI 2011A) data and the SSM flux prediction in SERENELLI 2011 (Astrophysical Journal 743 24 (2011)) with the exception that the ${}^{8}\mathrm {B}$ flux was left free.
|
20
GANDO 2011 obtain this result with three-neutrino fit using the KamLAND + solar data. Superseded by GANDO 2013 .
|
21
GANDO 2011 obtain this result with three-neutrino fit using the KamLAND data only. Superseded by GANDO 2013 .
|
22
AHARMIM 2010 global solar neutrino data include SNO's low-energy-threshold analysis survival probability day/night curves, SNO Phase III integral rates (AHARMIM 2008 ), Cl (CLEVELAND 1998 ), SAGE (ABDURASHITOV 2009 ), Gallex/GNO (HAMPEL 1999 , ALTMANN 2005 ), Borexino (ARPESELLA 2008A), SK-I zenith (HOSAKA 2006 ), and SK-II day/night spectra (CRAVENS 2008 ).
|
23
AHARMIM 2010 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data and KamLAND data (ABE 2008A). $\mathit CPT$ invariance is assumed.
|
24
AHARMIM 2010 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data.
|
25
AHARMIM 2010 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta $ fixed to $2.3 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino data and KamLAND data (ABE 2008A). $\mathit CPT$ invariance is assumed.
|
26
AHARMIM 2010 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta $ fixed to $2.3 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino data.
|
27
ABE 2008A obtained this result by a rate + shape + time combined geoneutrino and reactor two-neutrino fit for $\Delta $ and tan $^2\theta _{12}$, using KamLAND data only. Superseded by GANDO 2011 .
|
28
ABE 2008A obtained this result by means of a two-neutrino fit using KamLAND, Homestake, SAGE, GALLEX, GNO, SK (zenith angle and E-spectrum), the SNO $\chi {}^{2}$-map, and solar flux data. $\mathit CPT$ invariance is assumed. Superseded by GANDO 2011 .
|
29
The result given by AHARMIM 2008 is $\theta $ = ($34.4$ ${}^{+1.3}_{-1.2})^\circ{}$. This result is obtained by a two-neutrino oscillation analysis using solar neutrino data including those of Borexino (ARPESELLA 2008A) and Super-Kamiokande-I (HOSAKA 2006 ), and KamLAND data (ABE 2008A). $\mathit CPT$ invariance is assumed.
|
30
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using SK ${{\mathit \nu}_{{e}}}$ data, CC data from other solar neutrino experiments, and KamLAND data (ARAKI 2005 ). $\mathit CPT$ invariance is assumed.
|
31
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using the data from Super-Kamiokande, SNO (AHMAD 2002 and AHMAD 2002B), and KamLAND (ARAKI 2005 ) experiments. $\mathit CPT$ invariance is assumed.
|
32
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using the Super-Kamiokande and SNO (AHMAD 2002 and AHMAD 2002B) solar neutrino data.
|
33
The result given by AHARMIM 2005A is $\theta $ = ($33.9$ $\pm1.6)^\circ{}$. This result is obtained by a two-neutrino oscillation analysis using SNO pure deuteron and salt phase data, SK ${{\mathit \nu}_{{e}}}$ data, ${}^{}\mathrm {Cl}$ and ${}^{}\mathrm {Ga}$ CC data, and KamLAND data (ARAKI 2005 ). $\mathit CPT$ invariance is assumed. AHARMIM 2005A also quotes $\theta $ = ($33.9$ ${}^{+2.4}_{-2.2})^\circ{}$ as the error enveloping the 68$\%$ CL two-dimensional region. This translates into sin$^22 \theta $ = $0.86$ ${}^{+0.05}_{-0.06}$.
|
34
AHARMIM 2005A obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in figure 35a of AHARMIM 2005A. AHARMIM 2005A also quotes tan $^2\theta $ = $0.45$ ${}^{+0.09}_{-0.08}$ as the error enveloping the 68$\%$ CL two-dimensional region. This translates into sin$^22 \theta $ = $0.86$ ${}^{+0.05}_{-0.07}$.
|
35
ARAKI 2005 obtained this result by a two-neutrino oscillation analysis using KamLAND and solar neutrino data. $\mathit CPT$ invariance is assumed. The 1$\sigma $ error shown here is translated from the number provided by the KamLAND collaboration, tan $^2\theta $ = $0.40$ ${}^{+0.07}_{-0.05}$. The corresponding number quoted in ARAKI 2005 is tan $^2\theta $ = $0.40$ ${}^{+0.10}_{-0.07}$ (sin$^22 \theta $ = $0.82$ $\pm0.07$), which envelops the 68$\%$ CL two-dimensional region.
|
36
The result given by AHMED 2004A is $\theta $ = ($32.5$ ${}^{+1.7}_{-1.6})^\circ{}$. This result is obtained by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (EGUCHI 2003 ). $\mathit CPT$ invariance is assumed. AHMED 2004A also quotes $\theta $ = ($32.5$ ${}^{+2.4}_{-2.3})^\circ{}$ as the error enveloping the 68$\%$ CL two-dimensional region. This translates into sin$^22 \theta $ = $0.82$ $\pm0.06$.
|
37
AHMED 2004A obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in Fig. 5(a) of AHMED 2004A. The best-fit point is $\Delta \mathit m{}^{2}$ = $6.5 \times 10^{-5}$ eV${}^{2}$, tan $^2\theta $ = $0.40$ (sin$^22 \theta $ = $0.82$).
|
38
The result given by SMY 2004 is tan $^2\theta $ = $0.44$ $\pm0.08$. This result is obtained by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (IANNI 2003 ). $\mathit CPT$ invariance is assumed.
|
39
SMY 2004 obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The 1$\sigma $ errors are read from Fig. 6(a) of SMY 2004 .
|
40
SMY 2004 obtained this result by a two-neutrino oscillation analysis using the Super-Kamiokande and SNO (AHMAD 2002 and AHMAD 2002B) solar neutrino data. The 1$\sigma $ errors are read from Fig. 6(a) of SMY 2004 .
|
41
AHMAD 2002B obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in Fig. 4(b) of AHMAD 2002B. The best fit point is $\Delta \mathit m{}^{2}$ = $5.0 \times 10^{-5}$ eV${}^{2}$ and tan $\theta $ = $0.34$ (sin$^22 \theta $ = 0.76).
|
42
FUKUDA 2002 obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in Fig. 4 of FUKUDA 2002 . The best fit point is $\Delta \mathit m{}^{2}$ = $6.9 \times 10^{-5}$ eV${}^{2}$ and tan $^2\theta $ = $0.38$ (sin$^22 \theta $ = 0.80).
|