Extended search for supernovalike neutrinos in NOvA coincident with LIGO/Virgo detections

Creators: Acero, M. A.; Adamson, P.; Aliaga, L.; 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.; Bernstein, R.; Bhatnagar, V.; Bhuyan, B.; Bian, J.; Blair, J.; Booth, A. C.; Bowles, R.; Bromberg, C.; Buchanan, N.; Butkevich, A.; Calvez, S.; Carroll, T. J.; Catano-Mur, E.; Choudhary, B. C.; Christensen, A.; 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.; Duyang, H.; Edayath, S.; Ehrlich, R.; Elkins, M.; Ewart, E.; Feldman, G. J.; Filip, P.; Franc, J.; Frank, M. J.; Gallagher, H. R.; Gandrajula, R. P.; Gao, F.; 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.; Hausner, H.; Heller, K.; Hewes, J.; Himmel, A.; Holin, A.; Huang, J.; Jargowsky, B.; Jarosz, J.; Jediny, F.; Johnson, C.; Judah, M.; Kakorin, I.; Kalra, D.; Kaplan, D. M.; Kalitkina, A.; Keloth, R.; Klimov, O.; Koerner, L. W.; Kolupaeva, L.; Kotelnikov, S.; Kralik, R.; Kullenberg, Ch.; Kubu, M.; Kumar, A.; Kuruppu, C. D.; Kus, V.; Lackey, T.; Lang, K.; Lasorak, P.; Lesmeister, J.; Lin, S.; Lister, A.; Liu, J.; Lokajicek, M.; Magill, S.; Manrique Plata, M.; 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.; Mu, W.; Mualem, L.; Muether, M.; Mufson, S.; Mulder, K.; Naples, D.; Nayak, N.; Nelson, J. K.; Nichol, R.; Niner, E.; Norman, A.; Norrick, A.; Nosek, T.; Oh, H.; Olshevskiy, A.; Olson, T.; Ott, J.; Paley, J.; Patterson, R. B.; Pawloski, G.; Petrova, O.; Petti, R.; Phan, D. D.; Plunkett, R. K.; Porter, J. C. C.; Rafique, A.; Psihas, F.; Raj, V.; Rajaoalisoa, M.; Ramson, B.; Rebel, B.; Rojas, P.; Ryabov, V.; Samoylov, O.; Sanchez, M. C.; Sánchez Falero, 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.; Swain, S.; Sweeney, C.; Tapia Oregui, B.; Tas, P.; Thakore, T.; Thayyullathil, R. B.; Thomas, J.; Tiras, E.; Tripathi, J.; Trokan-Tenorio, 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.; Wu, W.; Xiao, Y.; Yallappa Dombara, A.; Yonehara, K.; Yu, S.; Yu, Y.; Zadorozhnyy, S.; Zalesak, J.; Zhang, Y.; Zwaska, R.; NOvA Collaboration

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Abstract

A search is performed for supernovalike neutrino interactions coincident with 76 gravitational wave events detected by the LIGO/Virgo Collaboration. For 40 of these events, full readout of the time around the gravitational wave is available from the NOvA Far Detector. For these events, we set limits on the fluence of the sum of all neutrino flavors of F < 7(4)×10¹⁰ cm⁻² at 90% C.L. assuming energy and time distributions corresponding to the Garching supernova models with masses 9.6(27) M_⊙. Under the hypothesis that any given gravitational wave event was caused by a supernova, this corresponds to a distance of r > 29(50) kpc at 90% C.L. Weaker limits are set for other gravitational wave events with partial Far Detector data and/or Near Detector data.

Additional Information

© 2021 Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. Funded by SCOAP3. Received 10 June 2021; accepted 16 August 2021; published 15 September 2021. 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, the Ministry of Education and Science of the Russian Federation (RMES), RSF, and BASIS Foundation, Russia; CNPq and FAPEG, Brazil; STFC, UKRI, 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.

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Published - PhysRevD.104.063024.pdf

Accepted Version - 2106.06035.pdf

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