Electron energy spectra, fluxes, and day-night asymmetries of 8B solar neutrinos from measurements with NaCl dissolved in the heavy-water detector at the Sudbury Neutrino Observatory

By B. Aharmim, Neubauer, C. Mifflin, L. Stonehill, J. Leslie, A. Marino, Kos, J. Wilkerson, H. Fergani, S. Seibert and 134 more. 2005

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SUPERNOVA CONSTRAINTS AND SYSTEMATIC UNCERTAINTIES FROM THE FIRST THREE YEARS OF THE SUPERNOVA LEGACY SURVEY (2011, methodology): “We compute them using standard techniques (e.g., Aharmim et al. 2005): Csys, ij = K∑ k=1 ( ∂mmod i ∂Sk )( ∂mmod j ∂Sk ) (∆Sk) 2 (6) where the sum is over the K systematics Sk, ∆Sk is the size of each term (for example, the uncertainty in the zero point), and mmod is defined as in equation 2.”
Sterile neutrino oscillations: the global picture (2013, methodology): “data from all the Super-Kamiokande phases I–IV [128–131] and the data from the three phases of SNO [132–134], including the results on the low energy threshold analysis of the combined SNO phases I–III [135].”