Published October 5, 2020
| Accepted Version
Journal Article
Open
Supernova neutrino detection in NOvA
- Creators
- Acero, M. A.
- Adamson, P.
- Agam, G.
- Aliaga, L.
- Alion, T.
- Allakhverdian, V.
- Anfimov, N.
- Antoshkin, A.
- Arrieta-Diaz, E.
- Asquith, L.
- Aurisano, A.
- Back, A.
- Backhouse, C.
- Baird, M.
- Balashov, N.
- Baldi, P.
- Bambah, B. A.
- Bashar, S.
- Bays, K.
- Bending, S.
- Bernstein, R.
- Bhatnagar, V.
- Bhuyan, B.
- Bian, J.
- Blair, J.
- Booth, A. C.
- Bour, P.
- Bowles, R.
- Bromberg, C.
- Buchanan, N.
- Butkevich, A.
- Bychkov, V.
- Calvez, S.
- Carroll, T. J.
- Catano-Mur, E.
- Childress, S.
- Choudhary, B. C.
- Coan, T. E.
- Colo, M.
- Corwin, L.
- Cremonesi, L.
- Davies, G. S.
- Derwent, P. F.
- Ding, P.
- Djurcic, Z.
- Dolce, M.
- Doyle, D.
- Dueñas Tonguino, D.
- Dukes, E. C.
- Dung, P.
- Duyang, H.
- Edayath, S.
- Ehrlich, R.
- Elkins, M.
- Feldman, G. J.
- Filip, P.
- Flanagan, W.
- Franc, J.
- Frank, M. J.
- Gallagher, H. R.
- Gandrajula, R.
- Gao, F.
- Germani, S.
- Giri, A.
- Gomes, R. A.
- Goodman, M. C.
- Grichine, V.
- Groh, M.
- Group, R.
- Guo, B.
- Habig, A.
- Hakl, F.
- Hall, A.
- Hartnell, J.
- Hatcher, R.
- Hatzikoutelis, A.
- Heller, K.
- Hewes, J.
- Himmel, A.
- Holin, A.
- Howard, B.
- Huang, J.
- Hylen, J.
- Jediny, F.
- Johnson, C.
- Judah, M.
- Kakorin, I.
- Kalra, D.
- Kaplan, D. M.
- Keloth, R.
- Klimov, O.
- Koerner, L. W.
- Kolupaeva, L.
- Kotelnikov, S.
- Kubu, M.
- Kullenberg, Ch.
- Kumar, A.
- Kuruppu, C. D.
- Kus, V.
- Lackey, T.
- Lang, K.
- Li, L.
- Lin, S.
- Lister, A.
- Lokajicek, M.
- Luchuk, S.
- Magill, S.
- Mann, W. A.
- Marshak, M. L.
- Martinez-Casales, M.
- Matveev, V.
- Mayes, B.
- Méndez, D. P.
- Messier, M. D.
- Meyer, H.
- Miao, T.
- Miller, W. H.
- Mishra, S. R.
- Mislivec, A.
- Mohanta, R.
- Moren, A.
- Morozova, A.
-
Mualem, L.
- Muether, M.
- Mufson, S.
- Mulder, K.
- Murphy, R.
- Musser, J.
- Naples, D.
- Nayak, N.
- Nelson, J. K.
- Nichol, R.
- Nikseresht, G.
- Niner, E.
- Norman, A.
- Norrick, A.
- Nosek, T.
- Olshevskiy, A.
- Olson, T.
- Paley, J.
-
Patterson, R. B.
- Pawloski, G.
- Petrova, O.
- Petti, R.
- Plunkett, R. K.
- Psihas, F.
- Rafique, A.
- Raj, V.
- Ramson, B.
- Rebel, B.
- Rojas, P.
- Ryabov, V.
- Samoylov, O.
- Sanchez, M. C.
- Sánchez Falero, S.
- Seong, I. S.
- Shanahan, P.
- Sheshukov, A.
- Singh, P.
- Singh, V.
- Smith, E.
- Smolik, J.
- Snopok, P.
- Solomey, N.
- Sousa, A.
- Soustruznik, K.
- Strait, M.
- Suter, L.
- Sutton, A.
- Sweeney, C.
- Talaga, R. L.
- Tapia Oregui, B.
- Tas, P.
- Thayyullathil, R. B.
- Thomas, J.
- Tiras, E.
- Torbunov, D.
- Tripathi, J.
- Tsaris, A.
- Torun, Y.
- Urheim, J.
- Vahle, P.
- Vallari, Z.
- Vasel, J.
- Vokac, P.
- Vrba, T.
- Wallbank, M.
- Warburton, T. K.
- Wetstein, M.
- Whittington, D.
- Wickremasinghe, D. A.
- Wojcicki, S. G.
- Wolcott, J.
- Yallappa Dombara, A.
- Yonehara, K.
- Yu, S.
- Yu, Y.
- Zadorozhnyy, S.
- Zalesak, J.
- Zhang, Y.
- Zwaska, R.
Abstract
The NOvA long-baseline neutrino experiment uses a pair of large, segmented, liquid-scintillator calorimeters to study neutrino oscillations, using GeV-scale neutrinos from the Fermilab NuMI beam. These detectors are also sensitive to the flux of neutrinos which are emitted during a core-collapse supernova through inverse beta decay interactions on carbon at energies of O(10 MeV). This signature provides a means to study the dominant mode of energy release for a core-collapse supernova occurring in our galaxy. We describe the data-driven software trigger system developed and employed by the NOvA experiment to identify and record neutrino data from nearby galactic supernovae. This technique has been used by NOvA to self-trigger on potential core-collapse supernovae in our galaxy, with an estimated sensitivity reaching out to 10 kpc distance while achieving a detection efficiency of 23% to 49% for supernovae from progenitor stars with masses of 9.6 M_⊙ to 27 M_⊙, respectively.
Additional Information
© 2020 IOP Publishing Ltd and Sissa Medialab. Received 15 May 2020; Accepted 2 August 2020; Published 5 October 2020. This document was prepared by the NOvA collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract No. DE-AC02-07CH11359. This work was supported by the U.S. Department of Energy; the U.S. National Science Foundation; the Department of Science and Technology, India; the European Research Council; the MSMT CR, GA UK, Czech Republic; the RAS, RFBR, RMES, RSF, and BASIS Foundation, Russia; CNPq and FAPEG, Brazil; STFC, and the Royal Society, United Kingdom; and the state and University of Minnesota. We are grateful for the contributions of the staffs of the University of Minnesota at the Ash River Laboratory and of Fermilab.Attached Files
Accepted Version - 2005.07155.pdf
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Additional details
- Eprint ID
- 105895
- Resolver ID
- CaltechAUTHORS:20201007-130710951
- Department of Energy (DOE)
- DE-AC02-07CH11359
- NSF
- Department of Science and Technology (India)
- European Research Council (ERC)
- Ministry of Education, Youth and Sports (Czech Republic)
- Grantová Agentura České Republiky
- Russian Academy of Sciences
- Russian Foundation for Basic Research
- Ministry of Education and Science of the Russian Federation
- Russian Science Foundation
- BASIS Foundation
- Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)
- Fundação de Amparo à Pesquisa do Estado de Goiás (FAPEG)
- Science and Technology Facilities Council (STFC)
- Royal Society
- State of Minnesota
- University of Minnesota
- Created
-
2020-10-07Created from EPrint's datestamp field
- Updated
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2022-07-12Created from EPrint's last_modified field