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The different conditions in the Gran Sasso beam line compared to the WANF influence the sensitivity of TOSCA in terms of oscillation parameters. Table 4 shows all relevant parameters necessary for such a comparison.
Table 4: Comparison of beam line parameters
The numbers for the column ``Upgraded WANF'' have been derived from applying to the WANF the super-cycle shown in Figure 2, but with a FS replacing the FE. Therefore an additional protons per super-cycle can be sent to the neutrino target during the same cycle as the SE. Moreover, table 4 assumes a global efficiency of 50% rather than the 75% quoted in [1].
The annual proton yield in the NGS will be smaller than the one in the upgraded WANF assuming the same efficiencies for both beams. The neutrino interaction rate per proton will be smaller as a consequence of the larger distance between proton target and detector. For a detector setup as described in SPSC/I213 and a data taking period of 3 years, one expects 67% of charge current events in the NGS compared to the WANF. Using the tau sensitivity and background estimation of SPSC/I213, a sensitivity in mixing angle for large of is expected (to be compared with for the upgraded WANF).
For small the sensitivity improves due to the two times larger average flight length of the neutrinos. The minimal reachable improves from to .
The sensitivity ranges for TOSCA at the WANF and at NGS are illustrated in Figure 9. The present limits and the expected final results from CHORUS and NOMAD are shown as well.
Figure 9: TOSCA sensitivity for WANF and NGS