Nobel Lecture: Discovery of atmospheric neutrino oscillations^*

Figure 1

Zenith angle distributions for multi-GeV (a) $e$-like and (b) $\mu$-like events observed in Kamiokande ([26]). The solid histogram shows the predicted distributions without oscillations. Absolute normalization had an uncertainty of 20% to 30%.

Figure 2

Schematic view of the Super-Kamiokande detector.

Figure 3

Zenith angle distributions for multi-GeV atmospheric neutrino events presented at the 18th International Conference on Neutrino Physics and Astrophysics (Neutrino’98) by the Super-Kamiokande collaboration ([36]).

Figure 4

The final slide (summary slide) of the presentation by the Super-Kamiokande Collaboration at Nuetrino’98 ([36]).

Figure 5

Data/prediction as a function of $L/E_{\nu }$ from Super-Kamiokande ([20]).

Figure 6

Zenith angle distributions for the $\tau$-like events selected from the data observed in Super-Kamiokande ([5]). Circles with error bars show the data. Solid histograms show the Monte Carlo prediction with ${\nu }_{\mu }\to {\nu }_{\tau }$ oscillations but without the charged current ${\nu }_{\tau }$ interactions. The gray histograms show the fit result including the ${\nu }_{\tau }$ interactions.

Figure 7

Zenith angle distribution for multi-GeV $e$-like (left) and $\mu$-like (right) atmospheric neutrino events observed in Super-Kamiokande (2015).