Limits on Astrophysical Antineutrinos with the KamLAND Experiment
Limits on Astrophysical Antineutrinos with the KamLAND Experiment
复制标题
DOI：
10.3847/1538-4357/ac32c1
复制
发表时间：
2021-08
期刊：
影响因子：
--
通讯作者：
S. Abe;S. Asami;A. Gando;Y. Gando;T. Gima;A. Goto;T. Hachiya;K. Hata;S. Hayashida;K. Hosokawa;K. Ichimura;S. Ieki;H. Ikeda;K. Inoue;K. Ishidoshiro;Y. Kamei;N. Kawada;T. Kinoshita;Y. Kishimoto;M. Koga;N. Maemura;T. Mitsui;H. Miyake;K. Nakamura;R. Nakamura;H. Ozaki;T. Sakai;H. Sambonsugi;I. Shimizu;J. Shirai;K. Shiraishi;A. Suzuki;Y. Suzuki;A. Takeuchi;K. Tamae;K. Ueshima;Y. Wada;H. Watanabe;Y. Yoshida;Shuhei Obara;A. Ichikawa;A. Kozkov;D. Chernyak;Y. Takemoto;S. Yoshida;S. Umehara;K. Fushimi;S. Hirata;K. Nakamura;M. Yoshida;B. Berger;B. Fujikawa;J. Learned;J. Maricic;S. Axani;Z. Fu;J. Ouellet;L. Winslow;Y. Efremenko;H. Karwowski;D. Markoff;W. Tornow;A. Li;J. Detwiler;S. Enomoto;M. Decowski;C. Grant;S. Dell’Oro;T. O’Donnell
中科院分区：
文献类型：
--
作者：
S. Abe;S. Asami;A. Gando;Y. Gando;T. Gima;A. Goto;T. Hachiya;K. Hata;S. Hayashida;K. Hosokawa;K. Ichimura;S. Ieki;H. Ikeda;K. Inoue;K. Ishidoshiro;Y. Kamei;N. Kawada;T. Kinoshita;Y. Kishimoto;M. Koga;N. Maemura;T. Mitsui;H. Miyake;K. Nakamura;R. Nakamura;H. Ozaki;T. Sakai;H. Sambonsugi;I. Shimizu;J. Shirai;K. Shiraishi;A. Suzuki;Y. Suzuki;A. Takeuchi;K. Tamae;K. Ueshima;Y. Wada;H. Watanabe;Y. Yoshida;Shuhei Obara;A. Ichikawa;A. Kozkov;D. Chernyak;Y. Takemoto;S. Yoshida;S. Umehara;K. Fushimi;S. Hirata;K. Nakamura;M. Yoshida;B. Berger;B. Fujikawa;J. Learned;J. Maricic;S. Axani;Z. Fu;J. Ouellet;L. Winslow;Y. Efremenko;H. Karwowski;D. Markoff;W. Tornow;A. Li;J. Detwiler;S. Enomoto;M. Decowski;C. Grant;S. Dell’Oro;T. O’Donnell
我们报道了用KamLAND探测器在8.3-30.8 MeV的中微子能量范围内搜索来自天体物理源的电子反中微子（ν¯e）。在6.72 kt年的液体闪烁体暴露中，我们通过反β衰变反应观察到18个候选事件。虽然中性电流大气中微子相互作用有很大的背景不确定性，但我们发现没有明显超出背景模式预测。假设几个超新星遗迹中微子光谱，我们给出了在分析范围内60-110 cm−2 s−1（90%置信水平，CL）的通量上限，并给出了一个与模型无关的通量。我们还对轻暗物质对与中微子对的湮灭速率设定了限制。这些数据提高了8B太阳中微子转化为ν¯e的概率上限，假设ν¯e形状未扭曲，ν νe→ν¯e<3.5×10−5 （90% CL）。这相当于在分析能量范围内太阳ν¯e的通量为60 cm−2 s−1 （90% CL）。
We report on a search for electron antineutrinos ( ν¯e ) from astrophysical sources in the neutrino energy range 8.3–30.8 MeV with the KamLAND detector. In an exposure of 6.72 kton-year of the liquid scintillator, we observe 18 candidate events via the inverse beta decay reaction. Although there is a large background uncertainty from neutral current atmospheric neutrino interactions, we find no significant excess over background model predictions. Assuming several supernova relic neutrino spectra, we give upper flux limits of 60–110 cm−2 s−1 (90% confidence level, CL) in the analysis range and present a model-independent flux. We also set limits on the annihilation rates for light dark matter pairs to neutrino pairs. These data improve on the upper probability limit of 8B solar neutrinos converting into ν¯e , Pνe→ν¯e<3.5×10−5 (90% CL) assuming an undistorted ν¯e shape. This corresponds to a solar ν¯e flux of 60 cm−2 s−1 (90% CL) in the analysis energy range.