Abstract from the paper The Supernova Breakout Burst Detection Potential of Terrestrial Neutrino Detectors by Joshua Wallace, Adam Burrows, and Joshua Dolence (Ap.J. 817, 182, 2016;arXiv:1512.01338):

We calculate the distance-dependent performance of a few representative terrestrial neutrino detectors in detecting and measuring the properties of the electron-neutrino breakout burst light curve in a Galactic core-collapse supernova. The breakout burst is a signature phenomenon of core collapse and offers a probe into the stellar core through collapse and bounce. We examine cases of no neutrino oscillations and oscillations due to normal and inverted neutrino-mass hierarchies. For the normal hierarchy, other neutrino flavors emitted by the supernova overwhelm the electron-neutrino signal, making a detection of the breakout burst difficult. For the inverted hierarchy, some detectors at some distances should be able to see the breakout burst peak and measure its properties. For the inverted hierarchy, the maximum luminosity of the breakout burst can be measured at 10 kpc to accuracies of ~30% for Hyper-K and ~60% for DUNE. Super-K and JUNO lack the mass needed to make an accurate measurement. IceCube cannot sufficiently account for the other neutrino flavors to discern a clear electron-neutrino breakout burst signal. For the inverted hierarchy, the time of the maximum luminosity of the breakout burst can be measured in Hyper-K to an accuracy of ~3 ms at 7 kpc, in DUNE ~2 ms at 4 kpc, and JUNO and Super-K can measure the time of maximum luminosity to an accuracy of ~2 ms at 1 kpc. For the inverted hierarchy, a measurement of the maximum luminosity of the breakout burst could be used to differentiate between nuclear equations of state.

Click here for the 12 solar-mass Data file with Spectra at various Times:

Click here for the 15 solar-mass Data file with Spectra at various Times:

Click here for the 20 solar-mass Data file with Spectra at various Times:

Click here for the 25 solar-mass Data file with Spectra at various Times:

Click here for the electron-neutrino energy bin file:

Click here for the anti-electron-neutrino energy bin file:

Click here for the mu-(tau-)neutrino energy bin file:

Description of Data files:

These data have been generated by Wallace, Burrows, and Dolence (Ap.J. 817, 182, 2016; arXiv:1512.01338) using FORNAX (Skinner et al. 2016; Burrows et al. 2017; Radice et al. 2017; Skinner et al. 2018).

There are two types of files available. The files of the form *_energy_bins.txt provide the values for the energy bins of each neutrino type. The first commented line of each file has listed the minimum and maximum energies used in the energy groups, followed by two columns of data. The first column is the energy group bin center, and the second column is the energy group bin width. There are 40 energy groups There are three of these files, one for each neutrino type:

nue - electron neutrinos nua - anti-electron neutrinos nux - the "nu_x" neutrinos: muon and tau neutrions and their antiparticles

The other files, one for each of five progenitor models from Woosley & Heger (2007), are the spectra for each neutrino type for the corresponding progenitor model. Note that one of the files uses the Shen EOS, while the rest employ the Lattimer & Swesty 220 MeV EOS. Each file corresponds to a specific time in the simulation, as can be seen in the file names.

'nu_spectra.t_002.dat' is a file containing spectral data at a time 2 ms after the time of maximum energy luminosity.

'nu_spectra.t_n029.dat' is a file containing spectral data at a time 29 ms *before* the time of maximum energy luminosity. The 'n' prior to the number in the file name stands for 'negative'.

There are three columns in each file, corresponding to data for each neutrino type: electron, anti-electron, and "nu_x" neutrinos, in that order. There are 40 rows of data, corresponding to the 40 energy groups. The data are the energy luminosity (not flux) spectral density for the given neutrino type in the given energy bin.

*Note: The units are 10^51 erg/s/MeV*