• • • We do not use the following data for averages, fits, limits, etc. • • • 
$5.95$ ${}^{+0.75}_{0.71}$ ${}^{+0.28}_{0.30}$ 
^{ 1} 

SNO+ 
$5.68$ ${}^{+0.39}_{0.41}$ ${}^{+0.03}_{0.03}$ 
^{ 2} 

BORX 
$5.25$ $\pm0.16$ ${}^{+0.11}_{0.13}$ 
^{ 3} 

SNO 
$5.046$ ${}^{+0.159}_{0.152}$ ${}^{+0.107}_{0.123}$ 
^{ 4} 

SNO 
$5.54$ ${}^{+0.33}_{0.31}$ ${}^{+0.36}_{0.34}$ 
^{ 5} 

SNO 
$4.94$ $\pm0.21$ ${}^{+0.38}_{0.34}$ 
^{ 6} 

SNO 
$4.81$ $\pm0.19$ ${}^{+0.28}_{0.27}$ 
^{ 6} 

SNO 
$5.09$ ${}^{+0.44}_{0.43}$ ${}^{+0.46}_{0.43}$ 
^{ 7} 

SNO 
$5.44$ $\pm0.99$ 
^{ 8} 


^{1}
ANDERSON 2019 reports this result from the measured ${{\mathit \nu}_{{e}}}{{\mathit e}}$ elastic scattering rate using a 69.2 kton$\cdot{}$day (or 114.7 days) of exposure from May through December, 2017 during the SNO+ detector's water commissioning phase, assuming the neutrino mixing parameters given in PDG 2016 and a standard solar model given in BAHCALL 2005 .

^{2}
AGOSTINI 2018B obtained this result from the measured ${{\mathit \nu}_{{e}}}{{\mathit e}}$ elastic scattering rate over the period between January 2008 and December 2016, assuming the MSWLMA oscillation parameters derived by ESTEBAN 2017 . Assuming a highmetalicity standard solar model, the electron neutrino survival probability for the ${}^{8}\mathrm {B}$ solar neutrino is calculated to be $0.37$ $\pm0.08$.

^{3}
AHARMIM 2013 obtained this result from a combined analysis of the data from all three phases, SNOI, II, and III. The measurement of the ${}^{8}\mathrm {B}$ flux mostly comes from the NC signal, however, CC contribution is included in the fit.

^{4}
AHARMIM 2010 reports this result from a joint analysis of SNO Phase I+II data with the "effective electron kinetic energy" threshold of 3.5 MeV. This result is obtained with the assumption of unitarity, which relates the NC, CC, and ES rates. The data were fit with the free parameters directly describing the total ${}^{8}\mathrm {B}$ neutrino flux and the energydependent ${{\mathit \nu}_{{e}}}$ survival probability.

^{5}
AHARMIM 2008 reports the results from SNO Phase III measurement using an array of ${}^{3}\mathrm {He}$ proportional counters to measure the rate of NC interactions in heavy water, over the period between November 27, 2004 and November 28, 2006, corresponding to 385.17 live days. A simultaneous fit was made for the number of NC events detected by the proportional counters and the numbers of NC, CC, and ES events detected by the PMTs, where the spectral distributions of the ES and CC events were not constrained to the ${}^{8}\mathrm {B}$ shape.

^{6}
AHARMIM 2005A measurements were made with dissolved NaCl (0.195$\%$ by weight) in heavy water over the period between July 26, 2001 and August 28, 2003, corresponding to 391.4 live days, and update AHMED 2004A. The CC, ES, and NC events were statistically separated. In one method, the ${}^{8}\mathrm {B}$ energy spectrum was not constrained. In the other method, the constraint of an undistorted ${}^{8}\mathrm {B}$ energy spectrum was added for comparison with AHMAD 2002 results.

^{7}
AHMAD 2002 determined the total flux of active ${}^{8}\mathrm {B}$ solar neutrinos by directly measuring the neutralcurrent reaction, ${{\mathit \nu}_{{{{\mathit \ell}}}}}$ ${{\mathit d}}$ $\rightarrow$ ${{\mathit n}}{{\mathit p}}{{\mathit \nu}_{{{{\mathit \ell}}}}}$ , which is equally sensitive to ${{\mathit \nu}_{{e}}}$, ${{\mathit \nu}_{{\mu}}}$, and ${{\mathit \nu}_{{\tau}}}$. The complete description of the SNO Phase I data set is given in AHARMIM 2007 .

^{8}
AHMAD 2001 deduced the total flux of active ${}^{8}\mathrm {B}$ solar neutrinos by combining the SNO chargedcurrent result (AHMAD 2001 ) and the SuperKamiokande ${{\mathit \nu}}{{\mathit e}}$ elasticscattering result (FUKUDA 2001 ).
