Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Antineutrinos from Pre-supernova Emission
Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Antineutrinos from Pre-supernova Emission
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DOI：
10.3847/1538-4357/ab4883
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发表时间：
2019-08
期刊：
影响因子：
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通讯作者：
C. Simpson;C. Simpson;K. Abe;K. Abe;C. Bronner;Y. Hayato;Y. Hayato;M. Ikeda;H. Ito;K. Iyogi;J. Kameda;J. Kameda;Y. Kataoka;Y. Kato;Y. Kishimoto;Y. Kishimoto;L. Marti;M. Miura;M. Miura;S. Moriyama;S. Moriyama;T. Mochizuki;M. Nakahata;M. Nakahata;Y. Nakajima;Y. Nakajima;S. Nakayama;S. Nakayama;T. Okada;K. Okamoto;A. Orii;G. Pronost;H. Sekiya;H. Sekiya;M. Shiozawa;M. Shiozawa;Y. Sonoda;A. Takeda;A. Takeda;A. Takenaka;Hidekazu Tanaka;T. Yano;R. Akutsu;T. Kajita;T. Kajita;K. Okumura;K. Okumura;R. Wang;J. Xia;D. Bravo-Berguño;L. Labarga;P. Fernandez;F. Blaszczyk;C. Kachulis;E. Kearns;E. Kearns;J. Raaf;J. Stone;J. Stone;L. Wan;T. Wester;S. Sussman;S. Berkman;J. Bian;N. J. Griskevich;W. Kropp;S. Locke;S. Mine;M. Smy;M. Smy;H. Sobel;H. Sobel;V. Takhistov;P. Weatherly;K. Ganezer;J. Hill;J. Kim;I. Lim;R. Park;B. Bodur;K. Scholberg;K. Scholberg;C. Walter;C. Walter;A. Coffani;O. Drapier;M. Gonin;J. Imber;T. Mueller;P. Paganini;T. Ishizuka;Toshikazu Nakamura;J. Jang;K. Choi;J. Learned;S. Matsuno;R. P. Litchfield;A. Sztuc;Y. Uchida;M. Wascko;V. Berardi;N. Calabria;M. Catanesi;R. A. Intonti;E. Radicioni;G. Rosa;G. Collazuol;F. Iacob;L. Ludovici;Y. Nishimura;S. Cao;M. Friend;T. Hasegawa;T. Ishida;Tomio Kobayashi;T. Nakadaira;K. Nakamura;K. Nakamura;Y. Oyama;K. Sakashita;T. Sekiguchi;T. Tsukamoto;K. Abe;M. Hasegawa;Y. Isobe;H. Miyabe;Y. Nakano;T. Shiozawa;T. Sugimoto;A. Suzuki;Y. Takeuchi;Y. Takeuchi;A. Ali;Y. Ashida;T. Hayashino;S. Hirota;M. Jiang;T. Kikawa;M. Mori;K. Nakamura;T. Nakaya;T. Nakaya;R. Wendell;R. Wendell;L. Anthony;N. McCauley;A. Pritchard;K. Tsui;Y. Fukuda;Y. Itow;M. Murrase;T. Niwa;M. Taani;M. Tsukada;P. Mijakowski;K. Frankiewicz;C. Jung;Xin Li;J. Palomino;G. Santucci;C. Vilela;M. Wilking;C. Yanagisawa;D. Fukuda;M. Harada;K. Hagiwara;T. Horai;H. Ishino;S. Ito;Y. Koshio;Y. Koshio;M. Sakuda;Y. Takahira;C. Xu;Y. Kuno;L. Cook;L. Cook;D. Wark;D. Wark;F. Lodovico;S. M. Sedgwick;B. Richards;S. Zsoldos;Shin-Do Kim;R. Tacik;R. Tacik;M. Thiesse;L. Thompson;H. Okazawa;Y. Choi;K. Nishijima;M. Koshiba;M. Yokoyama;M. Yokoyama;A. Goldsack;A. Goldsack;K. Martens;M. Murdoch;B. Quilain;Y. Suzuki;M. Vagins;M. Vagins;M. Kuze;Y. Okajima;M. Tanaka;T. Yoshida;M. Ishitsuka;R. Matsumoto;K. Ohta;J. Martin;C. Nantais;Harukazu Tanaka;T. Towstego;M. Hartz;A. Konaka;P. Perio;S. Chen;B. Jamieson;J. Walker;A. Minamino;G. Pintaudi
中科院分区：
文献类型：
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作者：
C. Simpson;C. Simpson;K. Abe;K. Abe;C. Bronner;Y. Hayato;Y. Hayato;M. Ikeda;H. Ito;K. Iyogi;J. Kameda;J. Kameda;Y. Kataoka;Y. Kato;Y. Kishimoto;Y. Kishimoto;L. Marti;M. Miura;M. Miura;S. Moriyama;S. Moriyama;T. Mochizuki;M. Nakahata;M. Nakahata;Y. Nakajima;Y. Nakajima;S. Nakayama;S. Nakayama;T. Okada;K. Okamoto;A. Orii;G. Pronost;H. Sekiya;H. Sekiya;M. Shiozawa;M. Shiozawa;Y. Sonoda;A. Takeda;A. Takeda;A. Takenaka;Hidekazu Tanaka;T. Yano;R. Akutsu;T. Kajita;T. Kajita;K. Okumura;K. Okumura;R. Wang;J. Xia;D. Bravo-Berguño;L. Labarga;P. Fernandez;F. Blaszczyk;C. Kachulis;E. Kearns;E. Kearns;J. Raaf;J. Stone;J. Stone;L. Wan;T. Wester;S. Sussman;S. Berkman;J. Bian;N. J. Griskevich;W. Kropp;S. Locke;S. Mine;M. Smy;M. Smy;H. Sobel;H. Sobel;V. Takhistov;P. Weatherly;K. Ganezer;J. Hill;J. Kim;I. Lim;R. Park;B. Bodur;K. Scholberg;K. Scholberg;C. Walter;C. Walter;A. Coffani;O. Drapier;M. Gonin;J. Imber;T. Mueller;P. Paganini;T. Ishizuka;Toshikazu Nakamura;J. Jang;K. Choi;J. Learned;S. Matsuno;R. P. Litchfield;A. Sztuc;Y. Uchida;M. Wascko;V. Berardi;N. Calabria;M. Catanesi;R. A. Intonti;E. Radicioni;G. Rosa;G. Collazuol;F. Iacob;L. Ludovici;Y. Nishimura;S. Cao;M. Friend;T. Hasegawa;T. Ishida;Tomio Kobayashi;T. Nakadaira;K. Nakamura;K. Nakamura;Y. Oyama;K. Sakashita;T. Sekiguchi;T. Tsukamoto;K. Abe;M. Hasegawa;Y. Isobe;H. Miyabe;Y. Nakano;T. Shiozawa;T. Sugimoto;A. Suzuki;Y. Takeuchi;Y. Takeuchi;A. Ali;Y. Ashida;T. Hayashino;S. Hirota;M. Jiang;T. Kikawa;M. Mori;K. Nakamura;T. Nakaya;T. Nakaya;R. Wendell;R. Wendell;L. Anthony;N. McCauley;A. Pritchard;K. Tsui;Y. Fukuda;Y. Itow;M. Murrase;T. Niwa;M. Taani;M. Tsukada;P. Mijakowski;K. Frankiewicz;C. Jung;Xin Li;J. Palomino;G. Santucci;C. Vilela;M. Wilking;C. Yanagisawa;D. Fukuda;M. Harada;K. Hagiwara;T. Horai;H. Ishino;S. Ito;Y. Koshio;Y. Koshio;M. Sakuda;Y. Takahira;C. Xu;Y. Kuno;L. Cook;L. Cook;D. Wark;D. Wark;F. Lodovico;S. M. Sedgwick;B. Richards;S. Zsoldos;Shin-Do Kim;R. Tacik;R. Tacik;M. Thiesse;L. Thompson;H. Okazawa;Y. Choi;K. Nishijima;M. Koshiba;M. Yokoyama;M. Yokoyama;A. Goldsack;A. Goldsack;K. Martens;M. Murdoch;B. Quilain;Y. Suzuki;M. Vagins;M. Vagins;M. Kuze;Y. Okajima;M. Tanaka;T. Yoshida;M. Ishitsuka;R. Matsumoto;K. Ohta;J. Martin;C. Nantais;Harukazu Tanaka;T. Towstego;M. Hartz;A. Konaka;P. Perio;S. Chen;B. Jamieson;J. Walker;A. Minamino;G. Pintaudi
超新星探测是超级神冈（SK）实验的主要目标。 SK（SK-Gd）的下一阶段将在探测器中添加硫酸钆（Gd），这将提高探测器识别中子的能力。在核心塌陷超新星（CCSN）发生之前，在数小时的时间尺度内，来自恒星热核和弱核过程的中微子和反中微子通量将不断增加；其中一些可以在 SK-Gd 上检测到。这可以提供即将发生的 CCSN 的早期预警，比检测到核心塌陷产生的中微子早几个小时。电子反中微子检测将依赖于低于 SK 通常分析能量阈值的逆 β 衰变事件，因此 Gd 负载对于减少背景同时最大限度地提高检测效率至关重要。假设中微子质量排序正常，对于一颗质量为 15-25 个太阳质量、质量约为 200 pc 的恒星来说，在核心塌陷之前的最后 12 小时内可以检测到 200 多个事件，这颗恒星是距离地球最近的红超巨星 α-Ori（参宿四）的代表。按照每世纪 1 次的统计误报率，在核心塌陷前 10 小时即可检测到，SK-Gd 可以在最远 600 pc 之外检测到超新星前的恒星。在钆装载后，可以向天体物理学界提供超新星爆发前警报。
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 (CCSN) will be preceded by an increasing flux of neutrinos and antineutrinos, 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 imminent CCSN, hours earlier than the detection of the neutrinos from core collapse. Electron antineutrino detection will rely on inverse beta decay events below the usual analysis energy threshold of SK, so Gd loading is vital to reduce backgrounds while maximizing detection efficiency. Assuming normal neutrino mass ordering, more than 200 events could be detected in the final 12 hr before core collapse for a 15–25 solar mass star at around 200 pc, which is representative of the nearest red supergiant to Earth, α-Ori (Betelgeuse). At a statistical false alarm rate of 1 per century, detection could be up to 10 hr before core collapse, and a pre-supernova star could be detected by SK-Gd up to 600 pc away. A pre-supernova alert could be provided to the astrophysics community following gadolinium loading.