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tokens: that cosmic rays and high-energy neutrinos may be produced by the interaction of an energetic outflow ejected by the newly born compact object with the surrounding pulsar nebula or supernova remnant at a distance . An FRB could also be produced during this interaction or directly inside the ejected outflow. The resulting neutrino flux may be low, because at such a distance from the progenitor the density of the target medium for the photo-hadronic interaction is quite small. However, the delay between the production of the radio and the neutrino signal is not clear yet. For all the hadronic models considered in this discussion, it seems that detecting a neutrino signal from single FRB sources may be difficult, as most of the FRB hadronic model predictions remain orders of magnitude below the ANTARES neutrino detection threshold. However, the expected large number of FRBs over the entire sky may contribute to a diffuse flux that can be tested by a large-scale neutrino telescope. This possibility is discussed in the following section. 4.4 Contribution to the neutrino diffuse flux In 2013, the IceCube Collaboration reported the significant detection of a cosmic diffuse neutrino flux (Aartsen et al. 2013 ). To date, the sources responsible for this cosmic isotropic signal have not been clearly identified. Even though the first compelling evidence of a cosmic high-energy neutrino signal from the blazar TXS 0506 + 056 has been claimed by Aartsen et al. ( 2018a , b ), it is still not clear how important the contribution of the blazars is to the neutrino diffuse flux. In contrast, the GRB contribution to this diffuse flux has already been constrained to be less than 1 per cent (Aartsen et al. 2015d ). The population of FRBs may also contribute significantly, because their expected rate is high, (Champion et al. 2016 ). This hypothesis is tested here by computing the 90 per cent CL upper limit on the diffuse neutrino flux associated with FRBs. As before, the neutrino flux associated with FRB sources is assumed to have a power-law energy distribution with spectral indexes γ = 1.0, 2.0, 2.5. The derived diffuse upper limits depend on the assumed neutrino spectrum. Hence, where N FRB is the number of FRBs considered in this analysis and is the characteristic neutrino fluence normalized to 100 TeV, as defined in equation ( 2 ) of the combined neutrino spectrum from the 12 FRBs. The neutrino fluence limit has been computed at the 90 per cent confidence level by estimating the average ANTARES effective area over the 12 FRB events for the different spectral models: According to the ANTARES upper limit on the individual neutrino fluxes from the 12 selected FRBs (see Table 2 ), and assuming the last updated estimate on the all-sky FRB rate (Bhandari et al. 2018 ), one can obtain the upper limits on the quasi-diffuse flux normalized to E 0 = 100 TeV, , 2.0 and 0.7 for E −1.0 , E −2.0 and E −2.5 neutrino spectra respectively. The neutrino diffuse flux observed by