Search for electron antineutrinos associated with gravitational wave events GW150914 and GW151226 using KamLAND
KamLAND Collaboration, A. Gando, Y. Gando, T. Hachiya, A. Hayashi, S. Hayashida, H. Ikeda, K. Inoue, K. Ishidoshiro, Y. Karino, M. Koga, S. Matsuda, T. Mitsui, … 展开作者
KamLAND Collaboration, A. Gando, Y. Gando, T. Hachiya, A. Hayashi, S. Hayashida, H. Ikeda, K. Inoue, K. Ishidoshiro, Y. Karino, M. Koga, S. Matsuda, T. Mitsui, K. Nakamura, S. Obara, T. Oura, H. Ozaki, I. Shimizu, Y. Shirahata, J. Shirai, A. Suzuki, T. Takai, K. Tamae, Y. Teraoka, K. Ueshima, H. Watanabe, A. Kozolov, Y. Takemoto, S. Yoshida, K. Fushimi, A. Piepke, T. I. Banks, B. E. Berger, B. K. Fujikawa, T. O'Donnell, J. G. Learned, J. Maricic, M. Sakai, L. A. Winslow, E. Krupczak, J. Ouellet, Y. Efremenko, H. J. Karwowski, D. M. Markoff, W. Tornow, J. A. Detwiler, S. Enomoto, M. P. Decowski
备注：
11 pages, 4 figures, as published in ApJL. Updated to replace power law spectrum with Fermi Dirac spectrum
We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and the luminosity of the astrophysical sources.
We present the results of a time-coincident event search for low-energy electron antineutrinos in the KamLAND detector with gamma-ray bursts from the Gamma-ray Coordinates Network and Fermi Gamma-ray Burst Monitor. Using a variable coincidence time window of $\pm$500s plus the duration of each gamma-ray burst, no statistically significant excess above background is observed. We place the world's most stringent 90% confidence level upper limit on the electron antineutrino fluence below 17.5 MeV. Assuming a Fermi-Dirac neutrino energy spectrum from the gamma-ray burst source, we use the availabl…
We present the results of a search for MeV-scale electron antineutrino events in KamLAND in coincident with the 60 gravitational wave events/candidates reported by the LIGO/Virgo collaboration during their second and third observing runs. We find no significant coincident signals within a $\pm$ 500 s timing window from each gravitational wave and present 90% C.L. upper limits on the electron antineutrino fluence between $10^{8}$-$10^{13}\,{\mathrm cm^2}$ for neutrino energies in the energy range of 1.8-111 MeV.
We report the results of a search for MeV-scale astrophysical neutrinos in KamLAND presented as an excess in the number of coincident neutrino interactions associated with the publicly available high-energy neutrino datasets from the IceCube Neutrino Observatory. We find no statistically significant excess in the number of observed low-energy electron antineutrinos in KamLAND, given a coincidence time window of $\pm$500s, $\pm$1,000s, $\pm$3,600s, and $\pm$10,000s around each of the IceCube neutrinos. We use this observation to present limits from 1.8 MeV to 100 MeV on the electron antineutrin…
We report on a search for electron antineutrinos ($\barν_e$) from astrophysical sources in the neutrino energy range 8.3 to 30.8 MeV with the KamLAND detector. In an exposure of 6.72 kton-year of the liquid scintillator, we observe 18 candidate events via the inverse beta decay reaction. Although there is a large background uncertainty from neutral current atmospheric neutrino interactions, we find no significant excess over background model predictions. Assuming several supernova relic neutrino spectra, we give upper flux limits of 60--110 cm$^{-2}$ s$^{-1}$ (90% CL) in the analysis range and…
Search for Diffuse Supernova Neutrino Background in the Full KamLAND Dataset with Neural-Network-Based Event Classification
Research Center for Neutrino Science, Tohoku University（东北大学中微子科学研究中心）；Department of Human Science, Obihiro University of Agriculture and Veterinary Medicine（带广畜产大学人类科学学院）
We present the results of a search for core-collapse supernova neutrinos, using long-term KamLAND data from 2002 March 9 to 2020 April 25. We focus on the electron antineutrinos emitted from supernovae in the energy range of 1.8--111 MeV. Supernovae will make a neutrino event cluster with the duration of $\sim$10 s in the KamLAND data. We find no neutrino clusters and give the upper limit on the supernova rate as to be 0.15 yr$^{-1}$ with a 90% confidence level. The detectable range, which corresponds to a >95% detection probability, is 40--59 kpc and 65--81 kpc for core-collapse supernovae an…
Using data of the Baksan Underground Scintillation Telescope (BUST) we have made a search for muon neutrinos and antineutrinos with energies above 1 GeV coinciding with the gravitational wave event GW170817 that was recorded on August 17, 2017 by the Advanced LIGO and Advanced Virgo observatories. This is a first detection of the new type of events occurring as a result of a merger of two neutron stars in a binary system. A short gamma-ray burst GRB170817A accompanying this event is an evidence of particle acceleration in the source whose precise position was determined by detection of the sub…
Providing a possible connection between neutrino emission and gravitational-wave (GW) bursts is important to our understanding of the physical processes that occur when black holes or neutron stars merge. In the Daya Bay experiment, using data collected from December 2011 to August 2017, a search has been performed for electron-antineutrino signals coinciding with detected GW events, including GW150914, GW151012, GW151226, GW170104, GW170608, GW170814, and GW170817. We used three time windows of $\mathrm{\pm 10~s}$, $\mathrm{\pm 500~s}$, and $\mathrm{\pm 1000~s}$ relative to the occurrence of …
Neutrino Oscillations Within the Induced Gravitational Collapse Paradigm of Long Gamma-Ray Bursts
超新星（SNe）长伽马射线暴（GRB）的诱导引力坍缩（IGC）模型预言了超新星喷出物在中子星（NS）伴星上的超临界吸积过程会产生大量的中微子-反中微子（$ν\barν$）辐射。中微子发射的亮度可达$10^{57}$ MeV s $^{-1}$，平均中微子能量为20 MeV，中微子密度为$10^{31}$ cm $^{-3}$。沿着它们从NS表面附近向外的路径，这些中微子经历由中微子与电子密度比决定的味道转变。我们确定了吸积带上的中微子和电子，并利用它们计算了中微子味的演化。对于正常和倒置的中微子质量等级，并在双味形式主义（$ν_{e}ν_{x}$），我们估计最终的电子和非电子中微子的内容后，两个振荡过程：（1）中微子集体效应，由于中微子自相互作用的中微子密度占主导地位，（2）Mikheyev-Smirnov-Wolfenstein（MSW）的效果，其中电子密度占主导地位。我们发现，最终的中微子内容是由$\sim$ 55%（$\sim$ 62%）的电子中微子，即$ν_{e}+\barν_{e}$，正常（倒置）中微子质量等级。这项工作的结果是第一步，除了核心崩溃SNe的一个新的来源的天体物理学MeV中微子的特性，因此，值得进一步关注。
