Supernova Relic Neutrino Search at Super-Kamiokande
Supernova Relic Neutrino Search at Super-Kamiokande
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DOI：
10.1103/physrevd.85.052007
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发表时间：
2011-11
影响因子：
5
通讯作者：
The Bays;T. Iida;K. Abe;Y. Hayato;K. Iyogi;J. Kameda;Y. Koshio;L. Marti;M. Miura;S. Moriyama;M. Nakahata;S. Nakayama;Y. Obayashi;H. Sekiya;M. Shiozawa;Y. Suzuki;A. Takeda;Y. Takenaga;K. Ueno;K. Kajita;K. Kaneyuki;T. McLachlan;K. Okumura;L. K. Pik;K. Martens;M. Vagins;L. Labarga;E. Kearns;M. Litos;J. Raaf;J. Stone;L. Sulak;W. Kropp;S. Mine;C. Regis;A. Renshaw;M. Smy;H. Sobel;K. Ganezer;J. Hill;W. Keig;S. Cho;J. Jang;J. Kim;I. Lim;J. Albert;K. Scholberg;C. Walter;R. Wendell;T. Wongjirad;T. Ishizuka;S. Tasaka;J. Learned;S. Matsuno;S. Smith;T. Hasegawa;T. Ishida;T. Ishii;T. Kobayashi;T. Nakadaira;K. Nakamura;K. Nishikawa;Y. Oyama;K. Sakashita;T. Sekiguchi;T. Tsukamoto;A. Suzuki;Y. Takeuchi;M. Ikeda;K. Matsuoka;A. Minamino;A. Murakami;T. Nakaya;Y. Fukuda;Y. Itow;G. Mitsuka;M. Miyake;T. Tanaka;J. Hignight;J. Imber;C. Jung;I. Taylor;C. Yanagisawa;A. Kibayashi;H. Ishino;S. Mino;M. Sakuda;T. Mori-;H. Toyota;Y. Kuno;S. Kim;B. Yang;H. Okazawa;Y. Choi;K. Nishijima;M. Koshiba;Y. Totsuka;M. Yokoyama;Y. Heng;S. Chen;H. Zhang;Z. Yang;P. Mijakowski;K. Connolly;M. Dziomba;R. Wilkes
中科院分区：
文献类型：
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作者：
The Bays;T. Iida;K. Abe;Y. Hayato;K. Iyogi;J. Kameda;Y. Koshio;L. Marti;M. Miura;S. Moriyama;M. Nakahata;S. Nakayama;Y. Obayashi;H. Sekiya;M. Shiozawa;Y. Suzuki;A. Takeda;Y. Takenaga;K. Ueno;K. Kajita;K. Kaneyuki;T. McLachlan;K. Okumura;L. K. Pik;K. Martens;M. Vagins;L. Labarga;E. Kearns;M. Litos;J. Raaf;J. Stone;L. Sulak;W. Kropp;S. Mine;C. Regis;A. Renshaw;M. Smy;H. Sobel;K. Ganezer;J. Hill;W. Keig;S. Cho;J. Jang;J. Kim;I. Lim;J. Albert;K. Scholberg;C. Walter;R. Wendell;T. Wongjirad;T. Ishizuka;S. Tasaka;J. Learned;S. Matsuno;S. Smith;T. Hasegawa;T. Ishida;T. Ishii;T. Kobayashi;T. Nakadaira;K. Nakamura;K. Nishikawa;Y. Oyama;K. Sakashita;T. Sekiguchi;T. Tsukamoto;A. Suzuki;Y. Takeuchi;M. Ikeda;K. Matsuoka;A. Minamino;A. Murakami;T. Nakaya;Y. Fukuda;Y. Itow;G. Mitsuka;M. Miyake;T. Tanaka;J. Hignight;J. Imber;C. Jung;I. Taylor;C. Yanagisawa;A. Kibayashi;H. Ishino;S. Mino;M. Sakuda;T. Mori-;H. Toyota;Y. Kuno;S. Kim;B. Yang;H. Okazawa;Y. Choi;K. Nishijima;M. Koshiba;Y. Totsuka;M. Yokoyama;Y. Heng;S. Chen;H. Zhang;Z. Yang;P. Mijakowski;K. Connolly;M. Dziomba;R. Wilkes
使用 2853 天的实时数据进行了新的超级神冈探测器对超新星遗迹中微子的搜索。与 2003 年 Super-Kamiokande 结果相比，现在的灵敏度大大提高，该结果将通量限制设置为接近许多理论预测。这种更详细的分析包括各种改进，例如提高效率、降低能量阈值和扩展数据集。超新星遗迹中微子通量的新组合上限介于 2.8 至 $3.1{\overline{\ensuremath{\nu}}}_{e}\text{ }\text{ }{\mathrm{cm}}^{\ensuremath{-}2}\text{ }{\mathrm{s}}^{\ensuremath{-}1}g16\text{ }\text{ }\mathrm{MeV}$总正电子能量（17.3 MeV ${\mathrm{E}}_{\ensuremath{\nu}}$）。
A new Super-Kamiokande search for supernova relic neutrinos was conducted using 2853 live days of data. Sensitivity is now greatly improved compared to the 2003 Super-Kamiokande result, which placed a flux limit near many theoretical predictions. This more detailed analysis includes a variety of improvements such as increased efficiency, a lower energy threshold, and an expanded data set. New combined upper limits on supernova relic neutrino flux are between 2.8 and $3.1{\overline{\ensuremath{\nu}}}_{e}\text{ }\text{ }{\mathrm{cm}}^{\ensuremath{-}2}\text{ }{\mathrm{s}}^{\ensuremath{-}1}g16\text{ }\text{ }\mathrm{MeV}$ total positron energy (17.3 MeV ${\mathrm{E}}_{\ensuremath{\nu}}$).