Measurement of neutrino and antineutrino neutral-current quasielasticlike interactions on oxygen by detecting nuclear deexcitation 
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Abe, K.; Akutsu, R.; Ali, Ahmed Farag; Alt, C.; Andreopoulos, C.; Anthony, L. H. V.; Antonova, M.; Aoki, Shigeki; Ariga, A.; Ashida, Yosuke; Atkin, E. T.; Awataguchi, Y.; Ban, S.; Barbi, M.; Barker, G. J.; Barr, G.; Barry, C.; Batkiewicz-Kwasniak, M.; Beloshapkin, A.; Bench, F.; Berardi, V.; Berkman, S.; Berns, L.; Bhadra, S.; Bienstock, S.; Blondel, A.; Bolognesi, S.; Bourguille, B.; Boyd, S. B.; Brailsford, D.; Bravar, A.; Bravo-Berguño, D.; Bronner, C.; Bubak, A.; Avanzini, M. Buizza; Calcutt, J.; Campbell, T.; Cao, S.; Cartwright, S. L.; Catanesi, M. G.; Cervera, A.; Chappell, A.; Checchia, C.; Cherdack, D.; Chikuma, N.; Christodoulou, G.; Coleman, J. P.; Collazuol, G.; Cook, L.; Coplowe, D.; Cudd, A.; Dąbrowska, A.; Rosa, G. De; Dealtry, T.; Denner, P. F.; Dennis, Steve; Densham, C.; Lodovico, F. Di; Dokania, N.; Dolan, S.; Drapier, O.; Dumarchez, J.; Dunne, P.; Eklund, L.; Emery-Schrenk, S.; Ereditato, A.; Fernández, P.; Feusels, T.; Finch, A. J.; Fiorentini, G. A.; Fiorillo, G.; François, C.; Friend, M.; Fujii, Y.; Fujita, Ryuichi; Fukuda, Daisuke; Fukuda, R.; Fukuda, Y.; Gameil, K.; Giganti, C.; Golan, T.; Gonin, M.; Gorin, A.; Guigue, M.; Hadley, D. R.; Haigh, J. T.; Hamacher-Baumann, P.; Hartz, M.; Hasegawa, T.; Hastings, N. C.; Hayashino, T.; Hayato, Y.; Hiramoto, A.; Hogan, M.; Holeczek, J.; Van, N. T. Hong; Iacob, F.; Ichikawa, A. K.; Ikeda, M.; Ishida, Toru; Ishii, T.; Ishitsuka, M.; Iwamoto, K.; Izmaylov, A.; Jamieson, B.; Jenkins, S. J.; Jesús-Valls, C.; Jiang, M.; Johnson, S.; Jönsson, P.; Jung, C. K.; Kabirnezhad, M.; Kaboth, A. C.; Kajita, T.; Kakuno, H.; Kameda, J.; Karlen, D.; Kasetti, S. P.; Kataoka, Y.; Katori, T.; Kato, Y.; Kearns, E.; Khabibullin, M.; Khotjantsev, A.; Kikawa, T.; Kim, H.; Kim, J.; King, S.; Kisiel, J.; Knight, A.; Knox, A.; Kobayashi, T.; Koch, L.; Koga, T.; Konaka, A.; Kormos, L. L.; Koshio, Y.; Kowalik, K.; Kubo, H.; Kudenko, Y.; Kukita, N.; Kuribayashi, S.; Kurjata, R.; Kutter, T.; Kuze, M.; Labarga, L.; Łagoda, J.; Lamoureux, Mathieu; Laveder, M.; Lawe, M.; Licciardi, M.; Lindner, T.; Litchfield, R. P.; Liu, S. L.; Li, X.; Longhin, A.; Ludovici, L.; Lu, X.-G.; Lux, T.; Machado, L. N.; Magaletti, L.; Mahn, Kendall; Malek, M.; Manly, S.; Maret, L.; Marino, A. D.; Martin, J. F.; Maruyama, T.; Matsubara, T.; Matsushita, K.; Matveev, V.; Mavrokoridis, K.; Mazzucato, E.; McCarthy, M.; McCauley, N.; McFarland, K. S.; McGrew, C.; Mefodiev, A.; Metelko, C.; Mezzetto, M.; Minamino, A.; Mineev, O.; Mine, S.; Miura, M.; Molina-Bueno, L.; Moriyama, S.; Morrison, John H.; Mueller, T.; Munteanu, L.; Murphy, S.; Nagai, Y.; Nakadaira, T.; Nakahata, M.; Nakajima, Yasuhiro; Nakamura, Akihiko; Nakamura, K.; Nakamura, K.; Nakayama, S.; Nakaya, T.; Nakayoshi, K.; Nantais, C.; Ngoc, Tran Van; Niewczas, K.; Nishikawa, K.; Nishimura, Y.; Nonnenmacher, T. S.; Nova, F.; Novella, P.; Nowak, J.; Nugent, J. C.; O’Keeffe, H. M.; O’Sullivan, L.; Odagawa, T.; Okumura, K.; Okusawa, T.; Oser, S. M.; Owen, R. A.; Oyama, Y.; Palladino, V.; Palomino, J. L.; Paolone, V.; Parker, William C.; Paudyal, P.; Pavin, M.; Payne, D. J.; Penn, G. C.; Pickering, L.; Pidcott, C.; Guerra, E. S. Pinzon; Pistillo, C.; Popov, Б.; Porwit, K.; Posiadała-Zezula, M.; Pritchard, A.; Quilain, B.; Radermacher, T.; Radicioni, E.; Radics, B.; Ratoff, P. N.; Reinherz‐Aronis, E.; Riccio, C.; Rondio, E.; Roth, Stefan; Rubbia, A.; Ruggeri, A. C.; Rychter, A.; Sakashita, K.; Sánchez, F.; Schloesser, C. M.; Scholberg, K.; Schwehr, J.; Scott, M.; Seiya, Y.; Sekiguchi, T.; Sekiya, H.; Sgalaberna, D.; Shah, R.; Shaikhiev, A.; Shaker, F.; Shaykina, A.; Shiozawa, M.; Shorrock, William I.; Shvartsman, A.; Smirnov, A. Yu.; Smy, M. B.; Sobczyk, J. T.; Sobel, H. W.; Soler, F. J. P.; Sonoda, Y.; Steinmann, J.; Suvorov, S.; Suzuki, A.; Suzuki, Shoji; Suzuki, Y.; Sztuc, A. A.; Tada, M.; Tajima, M.; Takeda, Atsushi; Takeuchi, Y.; Tanaka, Hiroyuki; Tanaka, Hirohisa; Tanaka, Satoshi; Thompson, L. F.; Toki, W. H.; Touramanis, C.; Tsui, K. M.; Tsukamoto, T.; Tzanov, M.; Uchida, Y.; Uno, W.; Vagins, M. R.; Valder, S.; Vallari, Z.; Vargas, D.; Vasseur, G.; Vilela, C.; Vinning, W. G. S.; Vladisavljevic, T.; Volkov, Vadim; Wąchała, T.; Walker, John M.; Walsh, J.; Wang, Y.; Wark, D.; Wascko, M. O.; Weber, A.; Wendell, R.; Wilking, M. J.; Wilkinson, C.; Wilson, J. R.; Wilson, R. J.; Wood, K.; Wret, C.; Yamada, Y.; Yamamoto, K.; Yanagisawa, C.; Yang, G.; Yano, T.; Yasutome, K.; Yen, S.; Yershov, N.; Yokoyama, M.; Yoshida, Tadashi; Yu, M.; Zalewska, A.; Zalipska, J.; Заремба, К.; Zarnecki, George; Ziembicki, M.; Zimmerman, E. D.; Zito, M.; Zsoldos, S.; Zykova, A.

doi:10.1103/physrevd.100.112009

Cited by 22 publications

(12 citation statements)

References 60 publications

(94 reference statements)

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“…In the SRN search at SK, atmospheric neutrino backgrounds are classified into two as the neutral-current quasielastic (NCQE) interactions and the others (non-NCQE). NCQE interactions involve nuclear γ ray emission via primary neutrino and following neutron reactions (Abe et al 2019), which mimic the positron signal from IBD. Charged-current interactions of atmospheric electron antineutrinos give the exactly same final state as IBD.…”

Section: Mev)mentioning

confidence: 99%

“…On the other hand, we as-sume 30%, 20%, and 10% for HK 3 years, HK 5 years, and HK 10 years, respectively. 5 These are based on the expected efforts in accelerator neutrino and nuclear experiments as described in Abe et al (2019). In Abe et al (2021), the non-NCQE background was estimated by using the sideband region, whose uncertainty is then mostly statistical.…”

Section: Mev)mentioning

confidence: 99%

See 1 more Smart Citation

Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos

Ashida¹,

Nakazato²

2022

Preprint

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Core collapse of massive stars leads to the different fate for various physical factors, which gives different spectra of the emitted neutrinos. We focus on the supernova relic neutrinos (SRNs) as a probe to investigate the stellar collapse fate. We present the SRN fluxes and event rate spectra at a detector for three resultant states after stellar core collapse, the typical mass neutron star, the higher mass neutron star, or the failed supernova forming a black hole, based on different nuclear equations of state. Then possible SRN fluxes are formed as mixtures of the three components. We also show the expected sensitivities at the next-generation water-based Cherenkov detectors, SK-Gd and Hyper-Kamiokande, as constraining the mixture fractions. This study provides a practical example of extracting astrophysical constraints through the SRN measurement.

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Section: Mev)mentioning

confidence: 99%

Section: Mev)mentioning

confidence: 99%

Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos

Ashida¹,

Nakazato²

2022

Preprint

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show abstract

“…Diffuse Supernova Neutrino Background Search at Super-Kamiokande S. El Hedri the associated systematic uncertainties using T2K measurements from Ref. [6]. Conversely, non-NCQE backgrounds, mainly composed of electrons from invisible muon and pion decays, are evaluated using the 29.5−79.5 MeV region as a sideband.…”

Section: Pos(icrc2021)1139mentioning

confidence: 99%

Diffuse Supernova Neutrino Background Search at Super-Kamiokande

Hedri¹,

Ashida²,

Giampaolo³

2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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We present the results of a search for the Diffuse Supernova Neutrino Background (DSNB) at Super-Kamiokande (SK) that incorporates 22.5 × 2970 kton.days of data from its fourth datataking phase. Two analyses, with different energy regimes covering the 9.3−81.3 MeV antineutrino energy range, have been developed based on previous SK searches, with substantially improved background modeling and data reduction techniques. Moreover, a combined analysis of nearly 20 years of SK data has been performed, with a 90% C.L. sensitivity to the DSNB flux comparable to various DSNB predictions. No significant evidence for a DSNB signal has been observed, and both analyses set world-leading limits on the DSNB flux that can reach about 2.7 .cm −2 .s −1 for a wide range of models.

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“…In this section, we will focus primarily on the benefits of blip sub-grouping for performing MeV-scale single γ-ray spectroscopy in LArTPC events. This technique could be valuable for different purposes, such as low-energy LArTPC calibration [8] or tagging of final-state nuclei produced in neutrino or BSM interactions [68].…”

Section: Single γ-Ray Calibration and Spectroscopymentioning

confidence: 99%

Benefits of MeV-scale reconstruction capabilities in large liquid argon time projection chambers

Castiglioni,

Foreman,

Lepetic

et al. 2020

Preprint

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Using truth-level Monte Carlo simulations of particle interactions in a large volume of liquid argon, we demonstrate physics capabilities enabled by reconstruction of topologically compact and isolated low-energy features, or 'blips,' in large liquid argon time projection chamber (LArTPC) events. These features are mostly produced by electron products of photon interactions depositing ionization energy. The blip identification capability of the LArTPC is enabled by its unique combination of size, position resolution precision, and low energy thresholds. We show that consideration of reconstructed blips in LArTPC physics analyses can result in substantial improvements in calorimetry for neutrino and new physics interactions and for final-state particles ranging in energy from the MeV to the GeV scale. Blip activity analysis is also shown to enable discrimination between interaction channels and final-state particle types. In addition to demonstrating these gains in calorimetry and discrimination, some limitations of blip reconstruction capabilities and physics outcomes are also discussed.

show abstract

Measurement of neutrino and antineutrino neutral-current quasielasticlike interactions on oxygen by detecting nuclear deexcitation γ rays

Cited by 22 publications

References 60 publications

Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos

Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos

Diffuse Supernova Neutrino Background Search at Super-Kamiokande

Benefits of MeV-scale reconstruction capabilities in large liquid argon time projection chambers

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