Supernova electron-neutrino interactions with xenon in the nEXO detector

S. Hedges; S. Al Kharusi; E. Angelico; J. P. Brodsky; G. Richardson; S. Wilde; A. Amy; A. Anker; I. J. Arnquist; P. Arsenault; A. Atencio; I. Badhrees; J. Bane; V. Belov; E. P. Bernard; T. Bhatta; A. Bolotnikov; J. Breslin; P. A. Breur; E. Brown; T. Brunner; E. Caden; G. F. Cao; L. Q. Cao; D. Cesmecioglu; E. Chambers; B. Chana; S. A. Charlebois; D. Chernyak; M. Chiu; R. Collister; M. Cvitan; J. Dalmasson; T. Daniels; L. Darroch; R. Devoe; M. L. Di Vacri; Y. Y. Ding; M. J. Dolinski; B. Eckert; M. Elbeltagi; R. Elmansali; L. Fabris; W. Fairbank; J. Farine; N. Fatemighomi; B. Foust; Y. S. Fu; D. Gallacher; N. Gallice; W. Gillis; D. Goeldi; A. Gorham; R. Gornea; G. Gratta; Y. D. Guan; C. A. Hardy; M. Heffner; E. Hein; J. D. Holt; E. W. Hoppe; A. House; W. Hunt; A. Iverson; P. Kachru; A. Karelin; D. Keblbeck; A. Kuchenkov; K. S. Kumar; A. Larson; M. B. Latif; K. G. Leach; B. G. Lenardo; D. S. Leonard; H. Lewis; G. Li; Z. Li; C. Licciardi; R. Lindsay; R. MacLellan; S. Majidi; C. Malbrunot; P. Martel-Dion; J. Masbou; K. McMichael; M. Medina-Peregrina; B. Mong; D. C. Moore; J. Nattress; C. R. Natzke; X. E. Ngwadla; K. Ni; A. Nolan; S. C. Nowicki; J. C. Nzobadila Ondze; J. L. Orrell; G. S. Ortega; C. T. Overman; L. Pagani; H. Peltz Smalley; A. Peña-Perez; A. Perna; A. Piepke; T. Pinto Franco; A. Pocar; J. F. Pratte; H. Rasiwala; D. Ray; K. Raymond; S. Rescia; V. Riot; R. Ross; R. Saldanha; S. Sangiorgio; S. Schwartz; S. Sekula; J. Soderstrom; A. K. Soma; F. Spadoni; X. L. Sun; S. Thibado; A. Tidball; T. Totev; S. Triambak; R. H.M. Tsang; O. A. Tyuka; E. Van Bruggen; M. Vidal; S. Viel; M. Walent; Q. D. Wang; W. Wang; Y. G. Wang; M. Watts; M. Wehrfritz; W. Wei; L. J. Wen; U. Wichoski; X. M. Wu; H. Xu; H. B. Yang; L. Yang; M. Yu; M. Yvaine; O. Zeldovich; J. Zhao

doi:10.1103/PhysRevD.110.093002

Supernova electron-neutrino interactions with xenon in the nEXO detector

S. Hedges, S. Al Kharusi, E. Angelico, J. P. Brodsky, G. Richardson, S. Wilde, A. Amy, A. Anker, I. J. Arnquist, P. Arsenault, A. Atencio, I. Badhrees, J. Bane, V. Belov, E. P. Bernard, T. Bhatta, A. Bolotnikov, J. Breslin, P. A. Breur, E. BrownT. Brunner, E. Caden, G. F. Cao, L. Q. Cao, D. Cesmecioglu, E. Chambers, B. Chana, S. A. Charlebois, D. Chernyak, M. Chiu, R. Collister, M. Cvitan, J. Dalmasson, T. Daniels, L. Darroch, R. Devoe, M. L. Di Vacri, Y. Y. Ding, M. J. Dolinski, B. Eckert, M. Elbeltagi, R. Elmansali, L. Fabris, W. Fairbank, J. Farine, N. Fatemighomi, B. Foust, Y. S. Fu, D. Gallacher, N. Gallice, W. Gillis, D. Goeldi, A. Gorham, R. Gornea, G. Gratta, Y. D. Guan, C. A. Hardy, M. Heffner, E. Hein, J. D. Holt, E. W. Hoppe, A. House, W. Hunt, A. Iverson, P. Kachru, A. Karelin, D. Keblbeck, A. Kuchenkov, K. S. Kumar, A. Larson, M. B. Latif, K. G. Leach, B. G. Lenardo, D. S. Leonard, H. Lewis, G. Li, Z. Li, C. Licciardi, R. Lindsay, R. MacLellan, S. Majidi, C. Malbrunot, P. Martel-Dion, J. Masbou, K. McMichael, M. Medina-Peregrina, B. Mong, D. C. Moore, J. Nattress, C. R. Natzke, X. E. Ngwadla, K. Ni, A. Nolan, S. C. Nowicki, J. C. Nzobadila Ondze, J. L. Orrell, G. S. Ortega, C. T. Overman, L. Pagani, H. Peltz Smalley, A. Peña-Perez, A. Perna, A. Piepke, T. Pinto Franco, A. Pocar, J. F. Pratte, H. Rasiwala, D. Ray, K. Raymond, S. Rescia, V. Riot, R. Ross, R. Saldanha, S. Sangiorgio, S. Schwartz, S. Sekula, J. Soderstrom, A. K. Soma, F. Spadoni, X. L. Sun, S. Thibado, A. Tidball, T. Totev, S. Triambak, R. H.M. Tsang, O. A. Tyuka, E. Van Bruggen, M. Vidal, S. Viel, M. Walent, Q. D. Wang, W. Wang, Y. G. Wang, M. Watts, M. Wehrfritz, W. Wei, L. J. Wen, U. Wichoski, X. M. Wu, H. Xu, H. B. Yang, L. Yang, M. Yu, M. Yvaine, O. Zeldovich, J. Zhao

Research output: Contribution to journal › Article › peer-review

Abstract

Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-β decay detector (∼5 metric ton, 90% Xe136, 10% Xe134) 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.

Original language	English
Article number	093002
Journal	Physical Review D
Volume	110
Issue number	9
DOIs	https://doi.org/10.1103/PhysRevD.110.093002
State	Published - Nov 1 2024

Bibliographical note

Publisher Copyright:
© 2024 authors. Published by the American Physical Society.

ASJC Scopus subject areas

Nuclear and High Energy Physics

Access to Document

10.1103/PhysRevD.110.093002

Cite this

Hedges, S., Al Kharusi, S., Angelico, E., Brodsky, J. P., Richardson, G., Wilde, S., Amy, A., Anker, A., Arnquist, I. J., Arsenault, P., Atencio, A., Badhrees, I., Bane, J., Belov, V., Bernard, E. P., Bhatta, T., Bolotnikov, A., Breslin, J., Breur, P. A., ... Zhao, J. (2024). Supernova electron-neutrino interactions with xenon in the nEXO detector. Physical Review D, 110(9), Article 093002. https://doi.org/10.1103/PhysRevD.110.093002

@article{3d0c0e6e0eef4db09d89fca4c815aa80,

title = "Supernova electron-neutrino interactions with xenon in the nEXO detector",

abstract = "Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-β decay detector (∼5 metric ton, 90% Xe136, 10% Xe134) 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.",

author = "S. Hedges and {Al Kharusi}, S. and E. Angelico and Brodsky, {J. P.} and G. Richardson and S. Wilde and A. Amy and A. Anker and Arnquist, {I. J.} and P. Arsenault and A. Atencio and I. Badhrees and J. Bane and V. Belov and Bernard, {E. P.} and T. Bhatta and A. Bolotnikov and J. Breslin and Breur, {P. A.} and E. Brown and T. Brunner and E. Caden and Cao, {G. F.} and Cao, {L. Q.} and D. Cesmecioglu and E. Chambers and B. Chana and Charlebois, {S. A.} and D. Chernyak and M. Chiu and R. Collister and M. Cvitan and J. Dalmasson and T. Daniels and L. Darroch and R. Devoe and {Di Vacri}, {M. L.} and Ding, {Y. Y.} and Dolinski, {M. J.} and B. Eckert and M. Elbeltagi and R. Elmansali and L. Fabris and W. Fairbank and J. Farine and N. Fatemighomi and B. Foust and Fu, {Y. S.} and D. Gallacher and N. Gallice and W. Gillis and D. Goeldi and A. Gorham and R. Gornea and G. Gratta and Guan, {Y. D.} and Hardy, {C. A.} and M. Heffner and E. Hein and Holt, {J. D.} and Hoppe, {E. W.} and A. House and W. Hunt and A. Iverson and P. Kachru and A. Karelin and D. Keblbeck and A. Kuchenkov and Kumar, {K. S.} and A. Larson and Latif, {M. B.} and Leach, {K. G.} and Lenardo, {B. G.} and Leonard, {D. S.} and H. Lewis and G. Li and Z. Li and C. Licciardi and R. Lindsay and R. MacLellan and S. Majidi and C. Malbrunot and P. Martel-Dion and J. Masbou and K. McMichael and M. Medina-Peregrina and B. Mong and Moore, {D. C.} and J. Nattress and Natzke, {C. R.} and Ngwadla, {X. E.} and K. Ni and A. Nolan and Nowicki, {S. C.} and {Nzobadila Ondze}, {J. C.} and Orrell, {J. L.} and Ortega, {G. S.} and Overman, {C. T.} and L. Pagani and {Peltz Smalley}, H. and A. Pe{\~n}a-Perez and A. Perna and A. Piepke and {Pinto Franco}, T. and A. Pocar and Pratte, {J. F.} and H. Rasiwala and D. Ray and K. Raymond and S. Rescia and V. Riot and R. Ross and R. Saldanha and S. Sangiorgio and S. Schwartz and S. Sekula and J. Soderstrom and Soma, {A. K.} and F. Spadoni and Sun, {X. L.} and S. Thibado and A. Tidball and T. Totev and S. Triambak and Tsang, {R. H.M.} and Tyuka, {O. A.} and {Van Bruggen}, E. and M. Vidal and S. Viel and M. Walent and Wang, {Q. D.} and W. Wang and Wang, {Y. G.} and M. Watts and M. Wehrfritz and W. Wei and Wen, {L. J.} and U. Wichoski and Wu, {X. M.} and H. Xu and Yang, {H. B.} and L. Yang and M. Yu and M. Yvaine and O. Zeldovich and J. Zhao",

note = "Publisher Copyright: {\textcopyright} 2024 authors. Published by the American Physical Society.",

year = "2024",

month = nov,

day = "1",

doi = "10.1103/PhysRevD.110.093002",

language = "English",

volume = "110",

number = "9",

}

Hedges, S, Al Kharusi, S, Angelico, E, Brodsky, JP, Richardson, G, Wilde, S, Amy, A, Anker, A, Arnquist, IJ, Arsenault, P, Atencio, A, Badhrees, I, Bane, J, Belov, V, Bernard, EP, Bhatta, T, Bolotnikov, A, Breslin, J, Breur, PA, Brown, E, Brunner, T, Caden, E, Cao, GF, Cao, LQ, Cesmecioglu, D, Chambers, E, Chana, B, Charlebois, SA, Chernyak, D, Chiu, M, Collister, R, Cvitan, M, Dalmasson, J, Daniels, T, Darroch, L, Devoe, R, Di Vacri, ML, Ding, YY, Dolinski, MJ, Eckert, B, Elbeltagi, M, Elmansali, R, Fabris, L, Fairbank, W, Farine, J, Fatemighomi, N, Foust, B, Fu, YS, Gallacher, D, Gallice, N, Gillis, W, Goeldi, D, Gorham, A, Gornea, R, Gratta, G, Guan, YD, Hardy, CA, Heffner, M, Hein, E, Holt, JD, Hoppe, EW, House, A, Hunt, W, Iverson, A, Kachru, P, Karelin, A, Keblbeck, D, Kuchenkov, A, Kumar, KS, Larson, A, Latif, MB, Leach, KG, Lenardo, BG, Leonard, DS, Lewis, H, Li, G, Li, Z, Licciardi, C, Lindsay, R, MacLellan, R, Majidi, S, Malbrunot, C, Martel-Dion, P, Masbou, J, McMichael, K, Medina-Peregrina, M, Mong, B, Moore, DC, Nattress, J, Natzke, CR, Ngwadla, XE, Ni, K, Nolan, A, Nowicki, SC, Nzobadila Ondze, JC, Orrell, JL, Ortega, GS, Overman, CT, Pagani, L, Peltz Smalley, H, Peña-Perez, A, Perna, A, Piepke, A, Pinto Franco, T, Pocar, A, Pratte, JF, Rasiwala, H, Ray, D, Raymond, K, Rescia, S, Riot, V, Ross, R, Saldanha, R, Sangiorgio, S, Schwartz, S, Sekula, S, Soderstrom, J, Soma, AK, Spadoni, F, Sun, XL, Thibado, S, Tidball, A, Totev, T, Triambak, S, Tsang, RHM, Tyuka, OA, Van Bruggen, E, Vidal, M, Viel, S, Walent, M, Wang, QD, Wang, W, Wang, YG, Watts, M, Wehrfritz, M, Wei, W, Wen, LJ, Wichoski, U, Wu, XM, Xu, H, Yang, HB, Yang, L, Yu, M, Yvaine, M, Zeldovich, O & Zhao, J 2024, 'Supernova electron-neutrino interactions with xenon in the nEXO detector', Physical Review D, vol. 110, no. 9, 093002. https://doi.org/10.1103/PhysRevD.110.093002

TY - JOUR

T1 - Supernova electron-neutrino interactions with xenon in the nEXO detector

AU - Hedges, S.

AU - Al Kharusi, S.

AU - Angelico, E.

AU - Brodsky, J. P.

AU - Richardson, G.

AU - Wilde, S.

AU - Amy, A.

AU - Anker, A.

AU - Arnquist, I. J.

AU - Arsenault, P.

AU - Atencio, A.

AU - Badhrees, I.

AU - Bane, J.

AU - Belov, V.

AU - Bernard, E. P.

AU - Bhatta, T.

AU - Bolotnikov, A.

AU - Breslin, J.

AU - Breur, P. A.

AU - Brown, E.

AU - Brunner, T.

AU - Caden, E.

AU - Cao, G. F.

AU - Cao, L. Q.

AU - Cesmecioglu, D.

AU - Chambers, E.

AU - Chana, B.

AU - Charlebois, S. A.

AU - Chernyak, D.

AU - Chiu, M.

AU - Collister, R.

AU - Cvitan, M.

AU - Dalmasson, J.

AU - Daniels, T.

AU - Darroch, L.

AU - Devoe, R.

AU - Di Vacri, M. L.

AU - Ding, Y. Y.

AU - Dolinski, M. J.

AU - Eckert, B.

AU - Elbeltagi, M.

AU - Elmansali, R.

AU - Fabris, L.

AU - Fairbank, W.

AU - Farine, J.

AU - Fatemighomi, N.

AU - Foust, B.

AU - Fu, Y. S.

AU - Gallacher, D.

AU - Gallice, N.

AU - Gillis, W.

AU - Goeldi, D.

AU - Gorham, A.

AU - Gornea, R.

AU - Gratta, G.

AU - Guan, Y. D.

AU - Hardy, C. A.

AU - Heffner, M.

AU - Hein, E.

AU - Holt, J. D.

AU - Hoppe, E. W.

AU - House, A.

AU - Hunt, W.

AU - Iverson, A.

AU - Kachru, P.

AU - Karelin, A.

AU - Keblbeck, D.

AU - Kuchenkov, A.

AU - Kumar, K. S.

AU - Larson, A.

AU - Latif, M. B.

AU - Leach, K. G.

AU - Lenardo, B. G.

AU - Leonard, D. S.

AU - Lewis, H.

AU - Li, G.

AU - Li, Z.

AU - Licciardi, C.

AU - Lindsay, R.

AU - MacLellan, R.

AU - Majidi, S.

AU - Malbrunot, C.

AU - Martel-Dion, P.

AU - Masbou, J.

AU - McMichael, K.

AU - Medina-Peregrina, M.

AU - Mong, B.

AU - Moore, D. C.

AU - Nattress, J.

AU - Natzke, C. R.

AU - Ngwadla, X. E.

AU - Ni, K.

AU - Nolan, A.

AU - Nowicki, S. C.

AU - Nzobadila Ondze, J. C.

AU - Orrell, J. L.

AU - Ortega, G. S.

AU - Overman, C. T.

AU - Pagani, L.

AU - Peltz Smalley, H.

AU - Peña-Perez, A.

AU - Perna, A.

AU - Piepke, A.

AU - Pinto Franco, T.

AU - Pocar, A.

AU - Pratte, J. F.

AU - Rasiwala, H.

AU - Ray, D.

AU - Raymond, K.

AU - Rescia, S.

AU - Riot, V.

AU - Ross, R.

AU - Saldanha, R.

AU - Sangiorgio, S.

AU - Schwartz, S.

AU - Sekula, S.

AU - Soderstrom, J.

AU - Soma, A. K.

AU - Spadoni, F.

AU - Sun, X. L.

AU - Thibado, S.

AU - Tidball, A.

AU - Totev, T.

AU - Triambak, S.

AU - Tsang, R. H.M.

AU - Tyuka, O. A.

AU - Van Bruggen, E.

AU - Vidal, M.

AU - Viel, S.

AU - Walent, M.

AU - Wang, Q. D.

AU - Wang, W.

AU - Wang, Y. G.

AU - Watts, M.

AU - Wehrfritz, M.

AU - Wei, W.

AU - Wen, L. J.

AU - Wichoski, U.

AU - Wu, X. M.

AU - Xu, H.

AU - Yang, H. B.

AU - Yang, L.

AU - Yu, M.

AU - Yvaine, M.

AU - Zeldovich, O.

AU - Zhao, J.

PY - 2024/11/1

Y1 - 2024/11/1

N2 - Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-β decay detector (∼5 metric ton, 90% Xe136, 10% Xe134) 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.

AB - Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-β decay detector (∼5 metric ton, 90% Xe136, 10% Xe134) 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.

UR - http://www.scopus.com/inward/record.url?scp=85212942213&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85212942213&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.110.093002

DO - 10.1103/PhysRevD.110.093002

M3 - Article

AN - SCOPUS:85212942213

SN - 2470-0010

VL - 110

JO - Physical Review D

JF - Physical Review D

IS - 9

M1 - 093002

ER -

Supernova electron-neutrino interactions with xenon in the nEXO detector

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