Supernova neutrino detection in NOvA

Acero, Ma; 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, Ba; Bashar, S.; Bays, K.; Bending, S.; Bernstein, R.; Bhatnagar, V; Bhuyan, B.; Bian, J.; Blair, J.; Booth, Ac; Bour, P.; Bowles, R.; Bromberg, C.; Buchanan, N.; Butkevich, A.; Bychkov, V; Calvez, S.; Carroll, Tj; Catano-Mur, E.; Childress, S.; Choudhary, Bc; Coan, T.; Colo, M.; Corwin, L.; Cremonesi, L.; Davies, Gs; Derwent, Pf; Ding, P.; Djurcic, Z.; Dolce, M.; Doyle, D.; Tonguino, D.; Dukes, Ec; Dung, P.; Duyang, H.; Edayath, S.; Ehrlich, R.; Elkins, M.; Feldman, Gj; Filip, P.; Flanagan, W.; Franc, J.; Frank, Mj; Gallagher, Hr; Gandrajula, R.; Gao, F.; Germani, S.; Giri, A.; Gomes, Ra; Goodman, M.; 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.; Keloth, R.; Klimov, O.; Koerner, Lw; Kolupaeva, L.; Kotelnikov, S.; Kubu, M.; Kullenberg, Ch; Kumar, A.; Kuruppu, Cd; Kus, V; Lackey, T.; Lang, K.; Li, L.; Lin, S.; Lister, A.; Lokajicek, M.; Luchuk, S.; Magill, S.; Mann, Wa; Marshak, Ml; Martinez-Casales, M.; Matveev, V; Mayes, B.; Mendez, Dp; Messier, Md; Meyer, H.; Miao, T.; Miller, Wh; Mishra, Sr.; 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, Jk; Nichol, R.; Nikseresht, G.; Niner, E.; Norman, A.; Norrick, A.; Nosek, T.; Olshevskiy, A.; Olson, T.; Paley, J.; Patterson, Rb; Pawloski, G.; Petrova, O.; Petti, R.; Plunkett, Rk; Psihas, F.; Rafique, A.; Raj, V; Ramson, B.; Rebel, B.; Rojas, P.; Ryabov, V; Samoylov, O.; Sanchez, M.; Falero, S.; Seong, I.; 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.; Oregui, B.; Tas, P.; Thayyullathil, Rb; Thomas, J.; Tiras, EMRAH; Torbunov, D.; Tripathi, J.; Tsaris, A.; Torun, Y.; Urheim, J.; Vahle, P.; Vallari, Z.; Vasel, J.; Vokac, P.; Vrba, T.; Wallbank, M.; Warburton, T.; Wetstein, M.; Whittington, D.; Wickremasinghe, D.; Wojcicki, Sg; Wolcott, J.; Dombara, A.; Yonehara, K.; Yu, S.; Yu, Y.; Zadorozhnyy, S.; Zalesak, J.; Zhang, Y.; Zwaska, R.

doi:10.1088/1475-7516/2020/10/014

Supernova neutrino detection in NOvA

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Acero M., Adamson P., Agam G., Aliaga L., Alion T., Allakhverdian V., ...More

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, vol.2020, no.10, 2020 (SCI-Expanded)

Publication Type: Article / Article
Volume: 2020 Issue: 10
Publication Date: 2020
Doi Number: 10.1088/1475-7516/2020/10/014
Journal Name: JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Aerospace Database, INSPEC, zbMATH
Keywords: core-collapse supernovae, neutrino experiments, supernova neutrinos, BURST
Erciyes University Affiliated: No

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-circle dot to 27 M-circle dot, respectively.