In our analysis we took into account the full observational information: energy, time, and angle for all events. For each detector we included: background, dead time, biases, and an accurate treatment of efficiencies. Our study favors the existence of the accretion phase with a significance of 𝚫𝝌𝟐= 𝟖. 𝟗, in accordance with literature. We performed a systematic investigation of the likelihood profile for all parameters, which allowed us to understand the characteristics of the likelihood function and to estimate uncertainties and correlations independently of the Hessian approach; see figure as an example. Finally, to test the validity of our model, we performed a hypothesis test adopting the Cramer criterion for each cumulative distribution represented in the figures above, obtaining satisfactory results reported in the table on the right. The combined probability maximization of all experiments produces parameter estimates whose values are consistent with the expectations of the theory. The agreement with the temporal and energy distributions of the model is excellent; that with the angular distributions is suboptimal but still acceptable. We conclude that our model effectively describes the anti-neutrino burst of SN1987A, highlighting salient features of interest for astrophysics and future observations. The results will be published and detailed in a paper in the near future. Supernova 1987A (SN1987A) is a Type II event that occurred in the Large Magellanic Cloud, approximately 168,000 light-years from Earth. An associated neutrino emission was observed: three experiments, Kamiokande-II, IMB and Baksan, detected a total of 29 events in a time span of about 30 seconds. This provided general support for theoretical expectations, which predict neutrinos as the main source of energy release in a core-collapse supernova event. SN1987A continues to be a key object of study, as it is the only such phenomenon observed to date. We present a state-of-the-art analysis of the SN1987A data, which corrects certain inaccuracies of previous analyses and is based on a new modelling of the neutrino flux, more consistent with the expectations of astrophysical simulations. Riccardo Maria Bozza1,2, Vigilante Di Risi1, Giuseppe Matteucci1,2, Veronica Oliviero1,2, Giulia Ricciardi1,2, Francesco Vissani3,R 1 Department of Physics ‘E. Pancini’, University of Naples Federico II, Naples, Italy 2 Istituto Nazionale di Fisica Nucleare Napoli, Naples, Italy 3 Laboratori Nazionali del Gran Sasso (INFN), Assergi, Italy 4 Osservatorio Astronomico di Brera (INAF), Merate, Italy Riccardo Maria Bozza1,2, Vigilante Di Risi1, Giuseppe Matteucci1,2, Veronica Oliviero1,2, Giulia Ricciardi1,2, Francesco Vissani3,4 1 Department of Physics ‘E. Pancini’, University of Naples Federico II, Naples, Italy 2 Istituto Nazionale di Fisica Nucleare Napoli, Naples, Italy 3 Laboratori Nazionali del Gran Sasso (INFN), Assergi, Italy 4 Osservatorio Astronomico di Brera (INAF), Merate, Italy Image Credit: NASA, ESA, CSA, M. Matsuura (Cardiff University), R. Arendt (NASA’s Goddard Spaceflight Center & University of Maryland, Baltimore County), C. Fransson (Stockholm University), J. Larsson (KTH Royal Institute of Technology), A. Pagan (STScI) A recent model (Symmetry 2021, 13(10), 1851) parametrizes the temporal profile of the incoming anti-neutrino flux from a CCSN in two independent components: accretion and cooling, accounting for an initial ramp-up phase for both components, as predicted by supernovae models. According to the mentioned model, accretion and cooling can be described by a single function: We calculated the differential interaction rate for Kamiokande-II, Baksan and IMB and employed a global Bayesian approach to estimate the best fit parameters for the model. Our approach at analyzing the neutrino emission The results for Kamiokande-II Best Fit Parameters Best fit parameters are obtained by maximizing the likelihood function with reasonable constraints provided by