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tokens: detector, as a function of the neutrino energy E ν and of the source declination. In our analysis, we consider the IceCube effective area for time-dependent searches using muon neutrinos from point sources (Aartsen et al. 2014b ). The area for point sources is found using the results of Aartsen et al. ( 2015 ) and the link https://icecube.wisc.edu/science/data/PS-3years . The number of neutrinos expected from a source at distance of ∼1 Gpc is consistent with the upper limits found by IceCube as shown in He et al. ( 2018 ). 4 FRACTION OF SUPERNOVA OBSERVATIONS WITH DETECTED NEUTRINO COUNTERPART We now estimate the fraction f ν of CCSNe detected electromagnetically that will also be detected via high-energy neutrinos. We convolve N ( r ) with the frequency of occurrence of CCSNe as a function of redshift. Due to the shortness of the lifetime of the progenitors of CCSNe, typically a few million years, we can use star formation history as proxy of the history of the CCSN rate (e.g. Hopkins Beacom 2011 ; Madau Dickinson 2014 ). We find that the expected fraction of supernovae within distance r max that will have a detected astrophysical high-energy neutrino counterpart is where f b is the jet beaming factor, defined as the fraction of the sky in which the jet emits high-energy neutrinos, f jet is the fraction of CCSNe that produces jets, Poiss( k , λ) is the Poisson probability of measuring k for average value λ, and r max is the maximum luminosity distance out to which the CCSN can be detected optically. This fraction depends on the neutrino detection threshold through N ( r ) defined in equation ( 1 ). In this definition, we do not include the possibility that a background neutrino can be coincident by chance with the supernova, which we separately account for below. Here, we consider r max for two representative facilities for ongoing and future observations: the Zwicky Transient Facility (ZTF; Rauch 2019 ) and the Large Synoptic Survey Telescope (LSST; https://www.lsst.org/scientists/scibook ). For ZTF, we assume a magnitude limit of R ∼ 19 for a typical 30 s exposure (Bellm Kulkarni 2017 ; Rauch 2019 ). For LSST, we assume a magnitude limit of R ∼ 24 for a typical exposure of 2 × 15 s (Abell et al. 2009 ). After assuming an absolute magnitude at maximum for CCSNe of M = −17.5 (Patat et al. 1994 ), we find that they can be detected out to r ∼ 200 Mpc with ZTF, and out to r ∼ 1.5 Gpc with LSST. The cosmological effects are taken into account in the analysis. For the LSST case, the redshift effects become important. With these observational limits, using equation ( 2 ) and the model parameters (Model 1) Γ = 100, t = 100 s, and L = 10 51 erg s −1 , we find that a fraction of CCSNe detected by ZTF might produce neutrinos detectable with IceCube or Km3NET. For LSST, this fraction becomes . In order to check the effects of the model parameters on our results, we consider another set of model parameters (Model 2) like Γ = 100, t = 3.3 × 10 4 s,