Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Antineutrinos from Pre-supernova Emission

Simpson, C.; Abe, K.; Bronner, C.; Hayato, Y.; Ikeda, M.; Itô, Hiroshi; Iyogi, K.; Kameda, J.; Kataoka, Y.; Kato, Y.; Kishimoto, Y.; Marti, Ll.; Miura, Makoto; Moriyama, S.; Mochizuki, T.; Nakahata, M.; Nakajima, Yasuhiro; Nakayama, S.; Okada, Taku; Okamoto, Ken‐ichi; Orii, A.; Pronost, G.; Sekiya, H.; Shiozawa, M.; Sonoda, Y.; Takeda, Atsushi; Takenaka, A.; Tanaka, Hirohisa; Yano, T.; Akutsu, R.; Kajita, T.; Okumura, K.; Wang, R.; Xia, J.; Bravo-Berguño, D.; Labarga, L.; Fernández, P.; Blaszczyk, F. d. M.; Kachulis, C.; Kearns, E.; Raaf, J. L.; Stone, J. L.; Wan, L.; Wester, T.; Sussman, S.; Berkman, S.; Bian, J. M.; Griskevich, N. J.; Kropp, W. R.; Locke, S.; Mine, S.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Weatherly, P.; Ganezer, K. S.; Hill, J.; Kim, J. Y.; Lim, I. T.; Park, R. G.; Bodur, B.; Scholberg, K.; Walter, C. W.; Coffani, A.; Drapier, O.; Gonin, M.; Imber, J.; Mueller, T.; Paganini, P.; Ishizuka, T.; Nakamura, T.; Jang, J. S.; Choi, K.; Learned, J. G.; Matsuno, S.; Litchfield, R. P.; Sztuc, A. A.; Uchida, Y.; Wascko, M. O.; Berardi, V.; Calabria, N. F.; Catanesi, M. G.; Intonti, R. A.; Radicioni, E.; Rosa, G. De; Collazuol, G.; Iacob, F.; Ludovici, L.; Nishimura, Y.; Cao, S.; Friend, M.; Hasegawa, T.; Ishida, Toru; Kobayashi, T.; Nakadaira, T.; Nakamura, Kenzo; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Hasegawa, M.; Isobe, Yuki; Miyabe, H.; Nakano, Y.; Shiozawa, T.; Sugimoto, Takashi; Suzuki, A.; Takeuchi, Y.; Ali, Ahmed Farag; Ashida, Yosuke; Hayashino, T.; Hirota, S.; Jiang, M.; Kikawa, T.; Mori, M.; Nakamura, K.; Nakaya, T.; Wendell, R.; Anthony, L. H. V.; McCauley, N.; Pritchard, A.; Tsui, K. M.; Fukuda, Y.; Itow, Y.; Murrase, M.; Niwa, T.; Taani, M.; Tsukada, M.; Mijakowski, P.; Frankiewicz, K.; Jung, C. K.; Li, X.; Palomino, J. L.; Santucci, G.; Vilela, C.; Wilking, M. J.; Yanagisawa, C.; Fukuda, Daisuke; Harada, Masayuki; Hagiwara, Kaoru; Horai, T.; Ishino, H.; Ito, S.; Koshio, Y.; Sakuda, M.; Takahira, Y.; Xu, Chenyuan; Kuno, Y.; Cook, L.; Wark, D.; Lodovico, F. Di; Sedgwick, S. Molina; Richards, B.; Zsoldos, S.; Kim, S. B.; Tacik, R.; Thiesse, M.; Thompson, L. F.; Okazawa, H.; Choi, Y.; Nishijima, K.; Koshiba, M.; Yokoyama, M.; Goldsack, A.; Martens, K.; Murdoch, M.; Quilain, B.; Suzuki, Y.; Vagins, M. R.; Kuze, M.; Okajima, Y.; Tanaka, M.; Yoshida, Tadashi; Ishitsuka, M.; Matsumoto, R.; Ohta, Kouji; Martin, J. F.; Nantais, C.; Towstego, T.; Hartz, M.; Konaka, A.; Perio, P. de; Chen, S.; Jamieson, B.; Walker, John M.; Minamino, A.; Pintaudi, G.

doi:10.3847/1538-4357/ab4883

Cited by 47 publications

(38 citation statements)

References 49 publications

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“…Neutrino astronomy, in concert with stellar models, can probe the isotopic composition profiles in energy producing regions of the Sun (Borexino Collaboration et al 2018 and nearby (d  1 kpc) pre-supernova massive stars up to tens of hours before core collapse (e.g., Patton et al 2017;Simpson et al 2019;Mukhopadhyay et al 2020). Stellar seismology, also in concert with stellar models, can probe the elemental composition profiles in pulsating stars from the upper main sequence (e.g., Simón-Díaz et al 2018;Pedersen et al 2019;Balona & Ozuyar 2020) through the red giant branch (e.g., Hekker & Christensen-Dalsgaard 2017;Hon et al 2018) to WDs (e.g., Hermes et al 2017;Giammichele et al 2018;Córsico et al 2019;Bell et al 2019;Bischoff-Kim et al 2019;Althaus et al 2021).…”

Section: Introductionmentioning

confidence: 99%

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

Chidester

Timmes

Schwab

et al. 2021

ApJ

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We explore changes in the adiabatic low-order g-mode pulsation periods of 0.526, 0.560, and 0.729 M ⊙ carbon–oxygen white dwarf models with helium-dominated envelopes due to the presence, absence, and enhancement of 22Ne in the interior. The observed g-mode pulsation periods of such white dwarfs are typically given to 6−7 significant figures of precision. Usually white dwarf models without 22Ne are fit to the observed periods and other properties. The rms residuals to the ≃150−400 s low-order g-mode periods are typically in the range of σ rms ≲ 0.3 s, for a fit precision of σ rms/P ≲ 0.3%. We find average relative period shifts of ΔP/P ≃ ±0.5% for the low-order dipole and quadrupole g-mode pulsations within the observed effective temperature window, with the range of ΔP/P depending on the specific g-mode, abundance of 22Ne, effective temperature, and the mass of the white dwarf model. This finding suggests a systematic offset may be present in the fitting process of specific white dwarfs when 22Ne is absent. As part of the fitting processes involves adjusting the composition profiles of a white dwarf model, our study on the impact of 22Ne can provide new inferences on the derived interior mass fraction profiles. We encourage routinely including 22Ne mass fraction profiles, informed by stellar evolution models, to future generations of white dwarf model-fitting processes.

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Section: Introductionmentioning

confidence: 99%

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

Chidester

Timmes

Schwab

et al. 2021

ApJ

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“…Future experiments, such as DUNE [6], will incorporate an enhanced tracking capability for hadrons in the final state. Also, it is worth mentioning the SK-Gd project [7], that improves the detection and identification capabilities of neutrons by adding Gd salts to the SuperKamiokande water tank. Compared to inclusive experiments, where only the final lepton is detected, the additional information about the hadrons in the final state, viz.…”

Section: Introductionmentioning

confidence: 99%

Neutrino energy reconstruction from semi-inclusive samples

González-Jiménez,

Barbaro,

Caballero

et al. 2021

Preprint

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We study neutrino-nucleus charged-current reactions on finite nuclei for the situation in which an outgoing muon and a proton are detected in coincidence, i.e., we focus on semi-inclusive cross sections. We limit our attention to one-body current interactions (quasielastic scattering) and assess the impact of different nuclear effects in the determination of the neutrino energy. We identify the regions in phase space where the neutrino energy can be reconstructed relatively well, and study whether the cross section in those regions is significant. Our results indicate that it is possible to filter more than 50% of all events according to the muon and proton kinematics, so that for the DUNE and T2K fluxes the neutrino energy can be determined with an uncertainty of less than 1% and 3%, respectively. Furthermore, we find that the reconstructed neutrino energy does not depend strongly on how one treats the final-state interactions and is not much affected by the description of the initial state. On the other hand, the estimations of the uncertainty on the neutrino energy show important sensitivity to the modeling of the initial state.

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“…ν e +p → e + +n (IBD) and the elastic (anti)neutrino-electron scattering ν(ν)+e − → ν(ν)+e − (eES) are two relevant detection channels. Recently, a dedicated study performed by the Super-Kamiokande collaboration [26] shows that the pre-SN neutrinos can be successfully observed in the Gadolinium-doped detector of Super-Kamiokande via the IBD reaction, for which the delayed signal of γ rays from the neutron capture on gadolinium will also be recorded. In addition, the liquid-argon time-projection chamber (LAr-TPC) detector of DUNE [27] is particularly sensitive to electron neutrinos due to the charged-current interaction ν e + 40 Ar → e − + 40 K * .…”

Section: Introductionmentioning

confidence: 99%

Towards a complete reconstruction of supernova neutrino spectra in future large liquid-scintillator detectors

Li¹,

Li²,

Wang³

et al. 2018

Phys. Rev. D

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In this paper, we show how to carry out a relatively more realistic and complete reconstruction of supernova neutrino spectra in the future large liquid-scintillator detectors, by implementing the method of singular value decomposition with a proper regularization. For a core-collapse supernova at a distance of 10 kpc in the Milky Way, itsν e spectrum can be precisely determined from the inverse beta-decay processν e þ p → e þ þ n, for which a 20 kiloton liquid-scintillator detector with the resolution similar to the Jiangmen Underground Neutrino Observatory may register more than 5000 events. We have to rely predominantly on the elastic neutrino-electron scattering ν þ e − → ν þ e − and the elastic neutrino-proton scattering ν þ p → ν þ p for the spectra of ν e and ν x , where ν denotes collectively neutrinos and antineutrinos of all three flavors and ν x for ν μ and ν τ as well as their antiparticles. To demonstrate the validity of our approach, we also attempt to reconstruct the neutrino spectra by using the time-integrated neutrino data from the latest numerical simulations of delayed neutrino-driven supernova explosions.

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Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Antineutrinos from Pre-supernova Emission

Cited by 47 publications

References 49 publications

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

Neutrino energy reconstruction from semi-inclusive samples

Towards a complete reconstruction of supernova neutrino spectra in future large liquid-scintillator detectors

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Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Antineutrinos from Pre-supernova Emission

Cited by 47 publications

References 49 publications

On the Impact of 22Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

On the Impact of 22Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

Neutrino energy reconstruction from semi-inclusive samples

Towards a complete reconstruction of supernova neutrino spectra in future large liquid-scintillator detectors

Contact Info

Product

Resources

About

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres