# Total Flux of Active ${}^{8}\mathrm {B}$ Solar Neutrinos INSPIRE search

Total flux of active neutrinos (${{\mathit \nu}_{{e}}}$, ${{\mathit \nu}_{{\mu}}}$, and ${{\mathit \nu}_{{\tau}}}$).

VALUE ($10^{6}$ cm${}^{-2}$s${}^{-1}$) DOCUMENT ID TECN  COMMENT
• • • We do not use the following data for averages, fits, limits, etc. • • •
$5.95$ ${}^{+0.75}_{-0.71}$ ${}^{+0.28}_{-0.30}$ 1
 2019
SNO+ Water phase; ${{\mathit \nu}_{{e}}}{{\mathit e}}$ scattering rate
$5.68$ ${}^{+0.39}_{-0.41}$ ${}^{+0.03}_{-0.03}$ 2
 2018 B
BORX From ${{\mathit \nu}_{{e}}}{{\mathit e}}$ scattering rate
$5.25$ $\pm0.16$ ${}^{+0.11}_{-0.13}$ 3
 2013
SNO All three phases combined
$5.046$ ${}^{+0.159}_{-0.152}$ ${}^{+0.107}_{-0.123}$ 4
 2010
SNO From ${{\mathit \phi}_{{NC}}}$ in Phase I+II, low threshold
$5.54$ ${}^{+0.33}_{-0.31}$ ${}^{+0.36}_{-0.34}$ 5
 2008
SNO $\phi _{NC}$ in Phase III
$4.94$ $\pm0.21$ ${}^{+0.38}_{-0.34}$ 6
 2005 A
SNO From ${{\mathit \phi}_{{NC}}}$; ${}^{8}\mathrm {B}$ shape not const.
$4.81$ $\pm0.19$ ${}^{+0.28}_{-0.27}$ 6
 2005 A
SNO From ${{\mathit \phi}_{{NC}}}$; ${}^{8}\mathrm {B}$ shape constrained
$5.09$ ${}^{+0.44}_{-0.43}$ ${}^{+0.46}_{-0.43}$ 7
 2002
SNO Direct measurement from ${{\mathit \phi}}_{\mathit NC}$
$5.44$ $\pm0.99$ 8
 2001
Derived from SNO+SuperKam, water Cherenkov
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 MSW-LMA oscillation parameters derived by ESTEBAN 2017 . Assuming a high-metalicity 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, SNO-I, 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 energy-dependent ${{\mathit \nu}_{{e}}}$ 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 neutral-current 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 charged-current result (AHMAD 2001 ) and the Super-Kamiokande ${{\mathit \nu}}{{\mathit e}}$ elastic-scattering result (FUKUDA 2001 ).
References:
 ANDERSON 2019
PR D99 012012 Measurement of the $^8$B solar neutrino flux in SNO+ with very low backgrounds
 AGOSTINI 2018B
NAT 562 505 Comprehensive measurement of $pp$-chain solar neutrinos
 AHARMIM 2013
PR C88 025501 Combined Analysis of all Three Phases of Solar Neutrino Data from the Sudbury Neutrino Observatory
 AHARMIM 2010
PR C81 055504 Low-Energy-Threshold Analysis of the Phase I and Phase II Data Sets of the Sudbury Neutrino Observatory
 AHARMIM 2008
PRL 101 111301 Independent Measurement of the Total Active ${}^{8}\mathrm {B}$ Solar Neutrino Flux Using an Array of ${}^{3}\mathrm {He}$ Proportional Counters at the Sudbury Neutrino Observatory
 AHARMIM 2005A
PR C72 055502 Search for Periodicities in the ${}^{8}\mathrm {B}$ Solar Neutrino Flux Measured by the Sudbury Neutrino Observatory
PRL 87 071301 Measurement of Charged Current Interactions Produced by ${}^{8}\mathrm {B}$ Solar Neutrinos at the SUDBURY Neutrino Observatory