Observing Supernova Neutrinos to Late Times Shirley Li

Observing Supernova Neutrinos to Late Times Shirley Li The Ohio State University Collaborators: Luke Roberts, John Beacom Te. VPA, August 2017

Timescale of a SN ? Detectable! Shirley Li (OSU) Figure credit: R. J. Hall 2/11

First input -- simulation Luke Roberts Blondin et al. , 2003 Shirley Li (OSU) 3/11

4/11

Late-time neutrinos Neutrino luminosity NS! Ø 1/t behavior Ø Transparency time Ø Connects SN and NS Preliminary Late-time neutrinos are interesting! Shirley Li (OSU) 5/11

Late-time neutrinos Neutrino energy Ø Moderate mixing effect Preliminary Late-time neutrinos are robust! Shirley Li (OSU) 6/11

Ø Inputs: • 10 kpc SN • 22. 5 kton • 3. 5 Me. V threshold Preliminary Plenty of events in Super-K! Shirley Li (OSU) 7/11

Other flavors Shirley Li (OSU) 8/11

Alternative outcome -- BH Different mechanisms for BH formation Preliminary BH may form at late times Shirley Li (OSU) 9/11

Detecting BH formation Detection significance of BH formation Preliminary We can detect BH formation at late times Shirley Li (OSU) 10/11

Conclusions Shirley Li (OSU) 11/11

Thank you!

Back up

Preliminary Easily reconstruct neutrino spectrum Shirley Li (OSU)

Ø Inputs: • 10 kpc SN • 40 kton • 5 Me. V threshold Preliminary Plenty of events to late time in DUNE! Shirley Li (OSU)

Preliminary Detection threshold needs to reach ~ 5 Me. V Shirley Li (OSU)

Ø Inputs: • 10 kpc SN • 22. 5 kton • 0. 1, 0. 2 Me. V threshold Preliminary Non-negligible events at late time Shirley Li (OSU)

Preliminary Detection threshold is crucial Shirley Li (OSU)