Observation in the Kamiokande-II detector of the neutrino burst from supernova SN1987A

Hirata, Keiko; Kajita, T.; Koshiba, M.; Nakahata, M.; Oyama, Y.; Sato, Nobuaki; Suzuki, A.; Takita, M.; Totsuka, Y.; Kifune, T.; Suda, T.; Takahashi, Keitaro; Tanimori, T.; Miyano, K.; Yamada, Masashi; Beier, E. W.; Feldscher, L. R.; Frati, W.; Kim, S. B.; Mann, A. K.; Newcomer, F. M.; Berg, R. Van; Zhang, W.; Cortez, B.

doi:10.1103/physrevd.38.448

Cited by 362 publications

(306 citation statements)

References 35 publications

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“…In Figure 1 we plot the average efficiencies for the KII, IMB, and Baksan detectors [2,4,6,49]. It is clear that the three detectors sample the signal quite differently.…”

Section: The Reported Datamentioning

confidence: 99%

“…This implies that the likelihood function is simply the product of independent probabilities for the detections and nondetections, 2) where N d is the number of detected events and j runs over all intervals for which no event was detected. As will become apparent, the number of nondetection intervals has no bearing on the analysis; only their total duration matters.…”

Section: Modeling Neutrino Detectionmentioning

confidence: 99%

“…The detection of neutrinos from supernova SN 1987A in the Large Magellanic Cloud by the Kamiokande II (KII) [1,2] Irvine-Michigan-Brookhaven (IMB) [3,4] and Baksan [5,6] detectors was a landmark event in astrophysics. Although only about two dozen of the ∼ 10 28 supernova neutrinos that passed through the Earth were detected, they provide us with our first glimpse of the collapsing core of a dying star, and hence deserve careful scrutiny.…”

Section: Introductionmentioning

confidence: 99%

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Bayesian analysis of neutrinos observed from supernova SN 1987A

2002

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We present a Bayesian analysis of the energies and arrival times of the neutrinos from supernova SN 1987A detected by the Kamiokande II, IMB, and Baksan detectors, and find strong evidence for two components in the neutrino signal: a long time scale component from thermal Kelvin-Helmholtz cooling of the nascent neutron star, and a brief (∼ 1 s), softer component similar to that expected from emission by accreting material in the delayed supernova scenario. In the context of this model, we show that the data constrain the electron antineutrino rest mass to be less than 5.7 eV with 95% probability. Our analysis takes advantage of significant advances that have occured in the years since the detections in both our understanding of the supernova mechanism and our ability to analyze sparse data. This has led to significant improvement over previous studies in two important respects. First, our comparison of the data with parameterized models of the neutrino emission uses a consistent and straightforward Bayesian statistical methodology. This methodology helps us distinguish the complementary tasks of parameter estimation and model assessment, and fully accounts for the strong, nonlinear correlations between inferred values of neutrino emission model parameters. It also clarifies and improves the derivation of the likelihood function (the probability for the data), improving on earlier derivations in two ways: more consistent accounting for the energy-dependent efficiencies of the detectors; and inclusion of the empirically measured detector background spectra. These improvements lead to significant differences between our inferences and those found in earlier studies. Inclusion of detector background spectra proves crucial for proper analysis of the Baksan data and for demonstrating its consistency with data from other detectors. Second, we compare the data with a much wider variety of neutrino emission models than was explored previously, several of them inspired by recent numerical calculations of collapse and explosion based on the delayed supernova mechanism. This allows us to compare predictions of both the prompt and delayed mechanisms with the data, and insures that our conclusions are robust. We find that two-component models for the neutrino signal are ∼ 100 times more probable than single-component models. Moreover, single-component models imply a radius and binding energy for the nascent neutron star significantly larger than those implied by even the stiffest acceptable equations of state for neutron star matter. In contrast, the radius and binding energy implied by two-component models are in agreement with predictions. Taking this agreement with prior expectations into account increases the odds in favor of two-component models by more than an order of magnitude. The inferred characteristics of the neutrino emission are in spectacular agreement with the salient features of the theory of stellar collapse and neutron star formation that had developed over several decades in the absence of direct observati...

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“…In Figure 1 we plot the average efficiencies for the KII, IMB, and Baksan detectors [2,4,6,49]. It is clear that the three detectors sample the signal quite differently.…”

Section: The Reported Datamentioning

confidence: 99%

Section: Modeling Neutrino Detectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Bayesian analysis of neutrinos observed from supernova SN 1987A

2002

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“…On February 23, 1987, a burst of mainly electron antineutrinos with energies of a few tens of MeV emitted by the supernova SN1987A was recorded simultaneously by the Baksan (Alekseev et al 1987), IMB (Bionta et al 1987), and Kamiokande-II (Hirata et al 1987(Hirata et al , 1988 detectors, a few hours before its optical counterpart was discovered. With just 24 neutrinos collected, stringent limits on the mass of theν e , its lifetime, its magnetic moment and the number of leptonic flavors could be derived (Kotake et al 2006).…”

Section: Introductionmentioning

confidence: 99%

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2011

A&A

137

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This paper describes the response of the IceCube neutrino telescope located at the geographic south pole to outbursts of MeV neutrinos from the core collapse of nearby massive stars. IceCube was completed in December 2010 forming a lattice of 5160 photomultiplier tubes that monitor a volume of ∼1 km 3 in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. Owing to subfreezing ice temperatures, the photomultiplier dark noise rates are particularly low. Hence IceCube can also detect large numbers of MeV neutrinos by observing a collective rise in all photomultiplier rates on top of the dark noise. With 2 ms timing resolution, IceCube can detect subtle features in the temporal development of the supernova neutrino burst. For a supernova at the galactic center, its sensitivity matches that of a background-free megaton-scale supernova search experiment. The sensitivity decreases to 20 standard deviations at the galactic edge (30 kpc) and 6 standard deviations at the Large Magellanic Cloud (50 kpc). IceCube is sending triggers from potential supernovae to the Supernova Early Warning System. The sensitivity to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to A109, page 1 of 18 detect the neutronization burst, a short outbreak of ν e 's released by electron capture on protons soon after collapse. Tantalizing signatures, such as the formation of a quark star or a black hole as well as the characteristics of shock waves, are investigated to illustrate IceCube's capability for supernova detection.

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“…Core collapse supernova modelers are now yearning for a Galactic explosion, to be able to compare the theoretically predicted neutrino signal from simulations with the actual measured one. So far SN1987A produced the only measured neutrino signal from a core collapse supernova event, which while providing very few data points, nevertheless enables scientists to probe the theoretically predicted scenario to a limited extent (see Hirata et al 1988).…”

Section: Introductionmentioning

confidence: 99%

The neutrino signal from protoneutron star accretion and black hole formation

Fischer

Whitehouse

Mezzacappa

et al. 2009

A&A

193

180

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Context. We discuss the formation of stellar mass black holes via protoneutron star (PNS) collapse. In the absence of an earlier explosion, the PNS collapses to a black hole due to the continued mass accretion onto the PNS. We present an analysis of the emitted neutrino spectra of all three flavors during the PNS contraction. Aims. Special attention is given to the physical conditions which depend on the input physics, e.g. the equation of state (EoS) and the progenitor model. Methods. The PNSs are modeled as the central object in core collapse simulations using general relativistic three-flavor Boltzmann neutrino transport in spherical symmetry. The simulations are launched from several massive progenitors of 40 M and 50 M . Results. We analyze the electron-neutrino luminosity dependencies and construct a simple approximation for the electron-neutrino luminosity, which depends only on the physical conditions at the electron-neutrinosphere. In addition, we analyze different (μ, τ)-neutrino pair-reactions separately and compare the differences during the post-bounce phases of failed core collapse supernova explosions of massive progenitors. We also investigate the connection between the increasing (μ, τ)-neutrino luminosity and the PNS contraction during the accretion phase before black hole formation. Conclusions. Comparing the different post bounce phases of the progenitor models under investigation, we find large differences in the emitted neutrino spectra. These differences and the analysis of the electron-neutrino luminosity indicate a strong progenitor model dependency of the emitted neutrino signal.

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Observation in the Kamiokande-II detector of the neutrino burst from supernova SN1987A

Cited by 362 publications

References 35 publications

Bayesian analysis of neutrinos observed from supernova SN 1987A

Bayesian analysis of neutrinos observed from supernova SN 1987A

IceCube sensitivity for low-energy neutrinos from nearby supernovae

The neutrino signal from protoneutron star accretion and black hole formation

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