Fig. 1. Drawing of the ICARUS T600 detector.

Fig. 2. Integral electron track energy spectrum generated from photon interaction.

Fig. 3. Fractional statistical error on total neutrino events collected in one year data taking vs. the main electron energy threshold.

Fig. 4. In the top an absorption event as generated by the GEANT Monte Carlo program is shown in two wire planes (U and V coordinates) put at an angle of 60°, the X-axis is the drift coordinate. The projected track length is about 3 cm, the main electron energy is 7 MeV, the associated energy is 2 MeV and the associated multiplicity is 3. In the bottom the same event is shown after digitisation. The grey scale of each pixel is proportional to the deposited charge. The resolution in the horizontal axis (drift direction) is 0.1 mm, and in the vertical axis is 3 mm (wire pitch).

Fig. 5. Fraction of elastic events (E>5 MeV) as a function of the cone angle within which the reconstructed electron direction in space is contained; the cone axis is defined by the parent neutrino direction. Three wire planes put at 60° angle and a 3 mm wire pitch are used.

Fig. 6. The ⁸B flux (right scale) is compared on the same energy scale with the average survival probabilities (left scale) for various MSW solutions.

Fig. 7. The spectral distortion due to the MSW effect is shown with BP98 undistorted ⁸B flux.

Fig. 8. Iso-R curves for active neutrinos. (b) is a blow up of the lower part of (a).

Fig. 9. Iso-R curves for sterile neutrinos.

Table 1. Main parameters of the readout chambers of the ICARUS detector

Table 2. Events per year and for 470 t liquid argon detector as a function of the kinetic energy threshold T_th

Table 3. Neutrino cross-sections as a function of the minimum accepted kinetic energy (T_th)

Table 4. Fraction of neutron capture events with at least one electron with kinetic energy greater than 5 MeV as a function of the associated energy and Compton electron multiplicity

Table 5. Fraction of neutrino elastic scattering events as a function of the associated energy and multiplicity. The data obtained after digitisation are used

Table 6. Fraction of Gamow–Teller events as a function of the associated energy and multiplicity. The data obtained after digitisation are used

Table 7. Fraction of pure Fermi events as a function of the associated energy and multiplicity. The data obtained after digitisation are used

Table 8. Expected number of events per year compared with the computed background rate. The numbers of events must be reduced by a factor ≈0.5, if we take into account the solar neutrino deficit revealed by experiments [5]

Table 9. The R-ratio range, the level of exclusion and the minimal exposure time for one module-year

Table 10. The one-sigma relative uncertainty for R as a function of the years of exposure time, together with the limits of the one-sigma exclusion region