Getting the most from the detection of Galactic supernova neutrinos in future large liquid-scintillator detectors

Future large liquid-scintillator detectors can be implemented to observe neutrinos from a core-collapse supernova in our Galaxy in various reaction channels: (1) the inverse beta decay [nu] sub(e)+ pn+ e super(+), (2) the elastic neutrino-proton scattering [nu] + p arrow right ][nu]+p, (3) the elastic neutrino-electron scattering [nu]+e super(-) arrow right [nu]+e super(-), (4) the charged-current [nu] sub(e) interaction [nu] sub(e)+ super(12) C arrow right e super(-)+ super(12) N, (5) the charged-current [nu] sub(e) interaction [nu] sub(e)+ super(12) C arrow right e super(+)+ super(12) B, and (6) the neutral-current interaction [nu]+ super(12) C arrow right [nu]+ super(12) C*. The less abundant super(13) C atoms in the liquid scintillator are also considered as a target, and both the charged-current interaction [nu] sub(e)+ super(13) C arrow right e super(-)+ super(13) N and the neutral-current interaction [nu]+ super(13) C arrow right [nu]+ super(13) C* are taken into account. In this work, we show for the first time that a global analysis of all these channels at a single liquid-scintillator detector, such as Jiangmen Underground Neutrino Observatory, is very important to test the average-energy hierarchy of supernova neutrinos and how the total energy is partitioned among neutrino flavors. In addition, the dominant channels for reconstructing neutrino spectra and the impact of other channels are discussed in great detail.