Supernova electron-neutrino interactions with xenon in the nEXO detector
Creators: name: NEXO Collaboration
name: Hedges, S.
name: Kharusi, S. Al
name: Angelico, E.
name: Brodsky, J. P.
name: Richardson, G.
name: Wilde, S.
name: Amy, A.
name: Anker, A.
name: Arnquist, I. J.
name: Arsenault, P.
name: Atencio, A.
name: Badhrees, I.
name: Bane, J.
name: Belov, V.
name: Bernard, E. P.
name: Bhatta, T.
name: Bolotnikov, A.
name: Breslin, J.
name: Breur, P. A.
name: Brown, E.
name: Brunner, T.
name: Caden, E.
name: Cao, G. F.
name: Cao, L. Q.
name: Cesmecioglu, D.
name: Chambers, E.
name: Chana, B.
name: Charlebois, S. A.
name: Chernyak, D.
name: Chiu, M.
name: Collister, R.
name: Cvitan, M.
name: Dalmasson, J.
name: Daniels, T.
name: Darroch, L.
name: DeVoe, R.
name: di Vacri, M. L.
name: Ding, Y. Y.
name: Dolinski, M. J.
name: Eckert, B.
name: Elbeltagi, M.
name: Elmansali, R.
name: Fabris, L.
name: Fairbank, W.
name: Farine, J.
name: Fatemighomi, N.
name: Foust, B.
name: Fu, Y. S.
name: Gallacher, D.
name: Gallice, N.
name: Gillis, W.
name: Goeldi, D.
name: Gorham, A.
name: Gornea, R.
name: Gratta, G.
name: Guan, Y. D.
name: Hardy, C. A.
name: Heffner, M.
name: Hein, E.
name: Holt, J. D.
name: Hoppe, E. W.
name: House, A.
name: Hunt, W.
name: Iverson, A.
name: Kachru, P.
name: Karelin, A.
name: Keblbeck, D.
name: Kuchenkov, A.
name: Kumar, K. S.
name: Larson, A.
name: Latif, M. B.
name: Leach, K. G.
name: Lenardo, B. G.
name: Leonard, D. S.
name: Lewis, H.
name: Li, G.
name: Li, Z.
name: Licciardi, C.
name: Lindsay, R.
name: MacLellan, R.
name: Majidi, S.
name: Malbrunot, C.
name: Martel-Dion, P.
name: Masbou, J.
name: McMichael, K.
name: Medina-Peregrina, M.
name: Mong, B.
name: Moore, D. C.
name: Nattress, J.
name: Natzke, C. R.
name: Ngwadla, X. E.
name: Ni, K.
name: Nolan, A.
name: Nowicki, S. C.
name: Ondze, J. C. Nzobadila
name: Orrell, J. L.
name: Ortega, G. S.
name: Overman, C. T.
name: Pagani, L.
name: Smalley, H. Peltz
name: Peña-Perez, A.
name: Perna, A.
name: Piepke, A.
name: Franco, T. Pinto
name: Pocar, A.
name: Pratte, J. -F.
name: Rasiwala, H.
name: Ray, D.
name: Raymond, K.
name: Rescia, S.
name: Riot, V.
name: Ross, R.
name: Saldanha, R.
name: Sangiorgio, S.
name: Schwartz, S.
name: Sekula, S.
name: Soderstrom, J.
name: Soma, A. K.
name: Spadoni, F.
name: Sun, X. L.
name: Thibado, S.
name: Tidball, A.
name: Totev, T.
name: Triambak, S.
name: Tsang, R. H. M.
name: Tyuka, O. A.
name: van Bruggen, E.
name: Vidal, M.
name: Viel, S.
name: Walent, M.
name: Wang, Q. D.
name: Wang, W.
name: Wang, Y. G.
name: Watts, M.
name: Wehrfritz, M.
name: Wei, W.
name: Wen, L. J.
name: Wichoski, U.
name: Wu, X. M.
name: Xu, H.
name: Yang, H. B.
name: Yang, L.
name: Yu, M.
name: Yvaine, M.
name: Zeldovich, O.
name: Zhao, J.
Publisher: name: arXiv
Year: 2024
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: High Energy Physics - Experiment (hep-ex)
subject: Nuclear Theory (nucl-th)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-$β$ decay detector (~5 metric ton, 90% ${}^{136}$Xe, 10% ${}^{134}$Xe) to evaluate its sensitivity to supernova neutrinos. Predictions for event rates and detectable signatures were modeled using the Model of Argon Reaction Low Energy Yields (MARLEY) event generator. We find good agreement between MARLEY's predictions and existing theoretical calculations of the inclusive cross sections at supernova neutrino energies. The interactions modeled by MARLEY were simulated within the nEXO simulation framework and were run through an example reconstruction algorithm to determine the detector's efficiency for reconstructing these events. The simulated data, incorporating the detector response, were used to study the ability of nEXO to reconstruct the incident electron-neutrino spectrum and these results were extended to a larger xenon detector of the same isotope enrichment. We estimate that nEXO will be able to observe electron-neutrino interactions with xenon from supernovae as far as 5-8 kpc from Earth, while the ability to reconstruct incident electron-neutrino spectrum parameters from observed interactions in nEXO is limited to closer supernovae.
description: 17 pages, 16 figures