Real-time supernova neutrino burst monitor at Super-Kamiokande

Abe, K.; Haga, Y.; Hayato, Y.; Ikeda, M.; Iyogi, K.; Kameda, J.; Kishimoto, Y.; Miura, Makoto; Moriyama, S.; Nakahata, M.; Nakano, Y.; Nakayama, S.; Sekiya, H.; Shiozawa, M.; Suzuki, Y.; Takeda, Atsushi; Tomura, T.; Ueno, K.; Wendell, R.; Yokozawa, T.; Irvine, T. J.; Kajita, T.; Kametani, I.; Kaneyuki, K.; Lee, K. P.; Mclachlan, T. C.; Nishimura, Y.; Richard, E.; Okumura, K.; Labarga, L.; Fernández, P.; Berkman, S.; Tanaka, Hirohisa; Tobayama, S.; Gustafson, J.; Kearns, E.; Raaf, J. L.; Stone, James L.; Sulak, L.; Goldhaber, M.; Carminati, G.; Kropp, W. R.; Mine, S.; Weatherly, P.; Renshaw, A.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Ganezer, K. S.; Hartfiel, B. L.; Hill, J.; Keig, W. E.; Hồng, Nguyễn Thị; Kim, J. Y.; Lim, I. T.; Akiri, T.; Himmel, A.; Scholberg, K.; Walter, C. W.; Wongjirad, T.; Ishizuka, T.; Tasaka, S.; Jang, J. S.; Learned, J. G.; Matsuno, S.; Smith, S. N.; Hasegawa, T.; Ishida, Toru; Ishii, T.; Kobayashi, T.; Nakadaira, T.; Nakamura, K.; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Suzuki, Akihiro; Takeuchi, Y.; Bronner, C.; Hirota, S.; Huang, K.; Ieki, K.; Kikawa, T.; Minamino, A.; Murakami, Akira; Nakaya, T.; Suzuki, K.; Takahashi, Sentaro; Tateishi, K.; Fukuda, Y.; Choi, K.; Itow, Y.; Mitsuka, G.; Mijakowski, P.; Hignight, J.; Imber, J.; Jung, C. K.; Yanagisawa, C.; Wilking, M. J.; Ishino, H.; Kibayashi, A.; Koshio, Y.; Mori, T.; Sakuda, M.; Yamaguchi, R.; Yano, T.; Kuno, Y.; Tacik, R.; Kim, S. B.; Okazawa, H.; Choi, Y.; Nishijima, K.; Koshiba, M.; Suda, Y.; Totsuka, Y.; Yokoyama, M.; Martens, K.; Marti, Ll.; Vagins, M. R.; Martin, J. F.; Perio, P. de; Konaka, A.; Chen, S.; Zhang, Y.; Connolly, K.; Wilkes, R. J.

doi:10.1016/j.astropartphys.2016.04.003

Cited by 84 publications

(83 citation statements)

References 37 publications

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“…This method of first-event selection reduces the σ t , as seen in Figure 3. The background rate in Super-K is approximately 0.01 Hz [8] for an energy threshold of 7 MeV, and error in the first-event method is low at this rate. However, the background rate may be much greater for future detectors.…”

Section: Effect Of Backgroundsmentioning

confidence: 91%

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Triangulation pointing to core-collapse supernovae with next-generation neutrino detectors

Linzer

Scholberg

2019

Phys. Rev. D

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A core-collapse supernova releases the vast majority of the gravitational binding energy of its compact remnant in the form of neutrinos over an interval of a few tens of seconds. In the event of a core-collapse supernova within our galaxy, multiple current and future neutrino detectors would see a large burst in activity. Neutrinos escape a supernova hours before light does, so any prompt information about the supernova's direction that can be inferred via the neutrino signal will help to enable early electromagnetic observations of the supernova. While there are methods to determine the direction via intrinsic directionality of some neutrino-matter interaction channels, a complementary method which will reach maturity with the next generation of large neutrino detectors is the use of relative neutrino arrival times at different detectors around the globe. To evaluate this triangulation method for realistic detector configurations of the next few decades, we generate random supernova neutrino signals with realistic detector assumptions, and quantify the error in expected time delay between detections. We investigate a practical and robust method of estimating the time differences between burst detections, also correcting for detection efficiency bias. With this method, we determine the pointing precision of supernova neutrino triangulation as a function of supernova distance and location, detectors used, detector background level and neutrino mass ordering assumption. Under favorable conditions, the 1σ supernova search area from triangulation could be reduced to a few percent of the sky. It should be possible to implement this method with low latency under realistic conditions.

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Section: Effect Of Backgroundsmentioning

confidence: 91%

“…Water-based Super-K and the planned Hyper-K employ Cherenkov radiation. Liquid scintillation detectors, in contrast, monitor scintillating compounds in liquid organic hydrocarbons that Super-K, which should yields few-degree pointing [8]. Pointing using fine-grained tracking in DUNE [38] is also very promising.…”

Section: Introductionmentioning

confidence: 99%

Triangulation pointing to core-collapse supernovae with next-generation neutrino detectors

Linzer

Scholberg

2019

Phys. Rev. D

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“…A detection of the GWs emitted in core collapse would be a milestone, revealing the inner mechanisms of core collapse and opening remarkable perspectives in multi-messenger astronomy. In particular, the neutrino emission which will be in coincidence, within few milliseconds, with the GW emission, should be detected by the current and future low energy neutrinos detectors (Super-K/Hyper-K [133], DUNE [134], JUNO [135], IceCube [136], the LVD [137], Borexino [138] and KamLAND [139]) with a higher signal to noise ratio than the GW signal and a very precise time resolution (few milliseconds) which is a fundamental information to search for a signal with low signal-to-noise ratio in the GW data. The false alarm rate of GW searches can be significantly improved with the temporal localization given by the neutrino signal.…”

Section: Multi-messenger Observations and Core Collapse Supernovaementioning

confidence: 99%

Science case for the Einstein telescope

Maggiore

Broeck

Bartolo

et al. 2020

J. Cosmol. Astropart. Phys.

978

730

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The Einstein Telescope (ET), a proposed European ground-based gravitationalwave detector of third-generation, is an evolution of second-generation detectors such as Advanced LIGO, Advanced Virgo, and KAGRA which could be operating in the mid 2030s. ET will explore the universe with gravitational waves up to cosmological distances. We discuss its main scientific objectives and its potential for discoveries in astrophysics, cosmology and fundamental physics. 1 1 Prepared for submission to the ESFRI Roadmap, on behalf of the ET steering committee.

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“…A near future detection of Galactic supernova ν e in large water Cherenkov detectors [65][66][67] or via triangulation [68] or via detection in large liquid scintillator detectors [69,70] can locate the supernova to a few degrees, however, that cannot improve this bound because of the lower energy of supernova neutrinos. Although electromagnetic observatories can point to a source with subdegree precision, yet this cannot obtain the best limit due to the much lower energy of photons involved.…”

mentioning

confidence: 99%

Constraints on neutrino speed, weak equivalence principle violation, Lorentz invariance violation, and dual lensing from the first high-energy astrophysical neutrino source TXS 0506+056

Laha

2019

Phys. Rev. D

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We derive some of the most stringent constraints on neutrino speed, weak equivalence principle violation, Lorentz invariance violation, and dual lensing from the first high-energy astrophysical neutrino source: TXS 0506+056. Observation of neutrino (IceCube-170922A) and photons in a similar time frame and from the same direction is used to derive these limits. All of these constraints are stronger than those obtained from the observation of SN 1987A. We describe ways in which these constraints can be further improved by orders of magnitude.

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Real-time supernova neutrino burst monitor at Super-Kamiokande

Cited by 84 publications

References 37 publications

Triangulation pointing to core-collapse supernovae with next-generation neutrino detectors

Triangulation pointing to core-collapse supernovae with next-generation neutrino detectors

Science case for the Einstein telescope

Constraints on neutrino speed, weak equivalence principle violation, Lorentz invariance violation, and dual lensing from the first high-energy astrophysical neutrino source TXS 0506+056

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