  In the first 10 seconds of a core-collapse supernova, almost all of its
progenitor's gravitational potential, O(10$^{53}$~ergs), is carried away in the
form of neutrinos. These neutrinos, with O(10~MeV) kinetic energy, can interact
via coherent elastic neutrino-nucleus scattering (CE$\nu$NS) depositing
O(1~keV) in detectors. In this work, we demonstrate that low-background dark
matter detectors, such as LUX-ZEPLIN (LZ), optimized for detecting low-energy
depositions, are capable of detecting these neutrino interactions. For
instance, a 27~M$_\odot$ supernova at 10~kpc is expected to produce $\sim$350
neutrino interactions in the 7-tonne liquid xenon active volume of LZ. Based on
the LS220 EoS neutrino flux model for a SN, the Noble Element Simulation
Technique (NEST), and predicted CE$\nu$NS cross-sections for xenon, to study
energy deposition and detection of SN neutrinos in LZ. We simulate the response
of the LZ data acquisition system (DAQ) and demonstrate its capability and
limitations in handling this interaction rate. We present an overview of the LZ
detector, focusing on the benefits of liquid xenon for supernova neutrino
detection. We discuss energy deposition and detector response simulations and
their results. We present an analysis technique to reconstruct the total number
of neutrinos and the time of the supernova core bounce.
