Speaker
Description
Astrophysical neutrinos are a great tool to study physics beyond the standard model of particle physics (BSM), one such source being galactic supernovae (SN). While these neutrinos can be detected by traditional neutrino detectors via the production of their charged lepton partners, they undergo the neutral current (NC) Coherent Elastic Neutrino Nucleus Scattering (CE$\nu$NS) process. These neutrinos, being typically of MeV energies, produce nuclear recoils (NRs), with kinetic energies of $E^2_\nu/M$, which are in the range of few to a few tens of keV. In addition, the coherent enhancement of the cross-section of the CE$\nu$NS process becomes particularly important in these energy ranges. Therefore, in order to detect these signals, detectors with very low thresholds and high nucleon number ($A$) are required. Large volume dual-phase liquid xenon TPCs, primarily designed to detect WIMPS, are therefore very suitable to detect such signals because of both very low backgrounds (as a result low thresholds) and high mass number. In this talk I will discuss the observable signals for SN neutrinos in xenon TPCs and the different backgrounds that affect these measurements. In this respect I will also discuss the possible limitations due to the charged-current (CC) interactions of the SN neutrinos.
