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

Atıf İçin Kopyala

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

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, cilt.2020, sa.10, 2020 (SCI-Expanded)

Yayın Türü: Makale / Tam Makale
Cilt numarası: 2020 Sayı: 10
Basım Tarihi: 2020
Doi Numarası: 10.1088/1475-7516/2020/10/014
Dergi Adı: JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Aerospace Database, INSPEC, zbMATH
Anahtar Kelimeler: core-collapse supernovae, neutrino experiments, supernova neutrinos, BURST
Erciyes Üniversitesi Adresli: Hayır

Özet

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.