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

@article{Simpson2019SensitivityOS,
  title={Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Anti-neutrinos from Pre-supernova Emission},
  author={C. Simpson and K. Abe and C. Bronner and Y. Hayato and M. Ikeda and H. Ito and K. Iyogi and J. Kameda and Y. Kataoka and Y. Kato and Y. Kishimoto and L. Marti and M. Miura and S. Moriyama and T. Mochizuki and M. Nakahata and Y. Nakajima and S. Nakayama and T. Okada and K. Okamoto and A. Orii and G. Pronost and H. Sekiya and M. Shiozawa and Y. Sonoda and A. Takeda and A. Takenaka and H. Tanaka and T. Yano and R. Akutsu and T. Kajita and K. Okumura and R. Wang and J. Xia and D. Bravo-Bergu{\~n}o and L. Labarga and P. Fern{\'a}ndez and F. Blaszczyk and C. Kachulis and E. Kearns and J. Raaf and J. Stone and L. Wan and T. Wester and S. Sussman and S. Berkman and J. Bian and N. J. Griskevich and W. Kropp and S. Locke and S. Mine and M. B. Smy and H. Sobel and V. Takhistov and P. Weatherly and K. S. Ganezer and J. Hill and J. Kim and I. Lim and R. G. Park and B. Bodur and K. Scholberg and C. Walter and A. Coffani and O. Drapier and M. Gonin and J. Imber and T. Mueller and P. Paganini and T. Ishizuka and T. Nakamura and J. S. Jang and K. Choi and J. Learned and S. Matsuno and R. P. Litchfield and A. Sztuc and Y. Uchida and M. Wascko and V. Berardi and N. F. Calabria and M. Catanesi and R. A. Intonti and E. Radicioni and G. Rosa and G. Collazuol and F. Iacob and L. Ludovici and Y. Nishimura and S. Cao and M. Friend and T. Hasegawa and T. Ishida and T. Kobayashi and T. Nakadaira and K. Nakamura and Y. Oyama and K. Sakashita and T. Sekiguchi and T. Tsukamoto and M. Hasegawa and Y. Isobe and H. Miyabe and Y. Nakano and T. Shiozawa and T. Sugimoto and A. T. Suzuki and Y. Takeuchi and A. Ali and Y. Ashida and T. Hayashino and S. Hirota and M. Jiang and T. Kikawa and M. Mori and T. Nakaya and R. Wendell and L. Anthony and N. McCauley and A. Pritchard and K. Tsui and Y. Fukuda and Y. Itow and M. Murrase and T. Niwa and M. Taani and M. Tsukada and P. Mijakowski and K. Frankiewicz and C. Jung and X. Li and J. Palomino and G. Santucci and C. Vilela and M. Wilking and C. Yanagisawa and D. Fukuda and M. Harada and K. Hagiwara and T. Horai and H. Ishino and S. Ito and Y. Koshio and M. Sakuda and Y. Takahira and C. Xu and Y. Kuno and L. Cook and D. Wark and F. Lodovico and S. M. Sedgwick and B. Richards and S. Zsoldos and S. Kim and R. Tacik and M. Thiesse and L. Thompson and H. Okazawa and Y. Choi and K. Nishijima and M. Koshiba and M. Yokoyama and A. Goldsack and K. Martens and M. Murdoch and B. Quilain and Y. Suzuki and M. Vagins and M. Kuze and Y. Okajima and M. Tanaka and T. Yoshida and M. Ishitsuka and R. Matsumoto and K. Ohta and J. Martin and C. M. Nantais and T. Towstego and M. Hartz and A. Konaka and P. Perio and S. Chen and B. Jamieson and J. Walker and A. Minamino and G. Pintaudi},
  journal={arXiv: High Energy Astrophysical Phenomena},
  year={2019}
}
Supernova detection is a major objective of the Super-Kamiokande (SK) experiment. In the next stage of SK (SK-Gd), gadolinium (Gd) sulfate will be added to the detector, which will improve the ability of the detector to identify neutrons. A core-collapse supernova will be preceded by an increasing flux of neutrinos and anti-neutrinos, from thermal and weak nuclear processes in the star, over a timescale of hours; some of which may be detected at SK-Gd. This could provide an early warning of an… Expand
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