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I derive an upper bound on the electron neutrino component of the diffusesupernova neutrino flux from the constraint on the antineutrino component atSuperKamiokande. The connection between antineutrino and neutrino channels isdue to the similarity of the muon and tau neutrino and antineutrino fluxesproduced in a supernova, and to the conversion of these species into electronneutrinos and antineutrinos inside the star. The limit on the electron neutrinoflux is 5.5 cm^-2 s^-1 above 19.3 MeV of neutrino energy, and is stronger thanthe direct limit from Mont Blanc by three orders of magnitude. It representsthe minimal sensitivity required at future direct searches, and is intriguinglyclose to the reach of the Sudbury Neutrino Observatory (SNO) and of the ICARUSexperiment. The electron neutrino flux will have a lower bound if the electronantineutrino flux is measured. Indicatively, the first can be smaller than thesecond at most by a factor of 2-3 depending on the details of the neutrinospectra at production.Comment: LaTeX, 5 pages, 1 figure. Paper is modified in the presentation (Fig.  1 was replaced with a different plot and Table 1 was expanded), with  unchanged results. References added and correcte

Diffuse neutrino flux from supernovae: Upper limit on the electron neutrino component from the nonobservation of antineutrinos at SuperKamiokande