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tokens: late times based on sophisticated simulations is presented in Mirizzi et al. ( 2016 ). In these studies the initial conditions have been prepared using other supernova models, thereby separating the PNS cooling from the explosion mechanism. In order to explore the connection between progenitors and compact objects using the neutrino signal, it is essential to study the long-term neutrino emission starting from the initial stellar model and include the thermal evolution of the PNS born in the resulting explosion. Evolution from the supernova explosion to the formation of a neutron star has been studied in 1D (Totani et al. 1998 ; Hüdepohl et al. 2010 ; Fischer et al. 2010 ) for selected progenitors and to a limited extent in 2D (Suwa 2014 ). 11 11 See Nakamura et al. ( 2015 ) and Horiuchi et al. ( 2018 ) for limitations of these models. Neutrino light curves in the 1D models by Totani et al. ( 1998 ) and Dalhed et al. ( 1999 ) have been routinely used to evaluate the total event number at neutrino detectors (see also Mirizzi et al. 2016 ). Due to limitations in the ability of these predictions and their focus on explosion dynamics, the expected number of neutrino events at underground neutrino detectors such as IceCube (Tamborra et al. 2013 ), Super-Kamiokande (Ikeda et al. 2007 ), and Hyper-Kamiokande (Abe et al. 2011 ; Hyper-Kamiokande Proto-Collaboration et al. 2018 ) has been estimated only for the dynamical phase using various models and numerical simulations to discuss these detectors’ ability to probe the physics of the supernova. As a result, the long-term behavior of the neutrino burst from the PNS has not been studied in detail with modern simulations covering a variety of progenitors. Our first aim in the current study is, therefore, to predict the basic features of the expected number of events at Super-Kamiokande for the full time sequence of supernova models. We utilize neutrino emission properties from a supernova neutrino database (Nakazato et al. 2013 ), which covers the complete dynamical evolution of the event from gravitational collapse to the cooling of the PNS. Through comparisons of event numbers for a set of progenitors systematically obtained from neutrino-radiation hydrodynamics (RHD) and PNS cooling simulations, we explore the differences in neutrino signals among models based on different progenitors. We discuss the time profile of the event rate for both early times around the bounce and the later phases of PNSs. We estimate the basic features of the event rate evolution for various models to assess whether one can extract information on the progenitor from future observations of a supernova neutrino burst. This is an important step in discussing the possibility of studying the progenitor’s mass, metallicity, and explosion timing, for instance, immediately after detection at Super-Kamiokande. Our second aim is to demonstrate the importance of the late phase of supernova neutrino emission. We study the long-term