Angular distribution of events from SN1987A

Bratton, C. B.; Casper, D.; Ciocio, A.; Claus, R.; Crouch, M. F.; Dye, S. T.; Errede, S.; Gajewski, W.; Goldhaber, M.; Haines, T. J.; Jones, T. W.; Kiełczewska, D.; Kropp, W. R.; Learned, J. G.; LoSecco, J. M.; Matthews, J.; Miller, R. S.; Mudan, M.; Price, L. R.; Reines, F.; Schultz, J.; Seidel, S. C.; Sinclair, D.; Sobel, H. W.; Stone, J. L.; Sulak, L.; Svoboda, R.; Thornton, G.; Velde, J. C. van der

doi:10.1103/physrevd.37.3361

Cited by 151 publications

(108 citation statements)

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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%

“…In Table II we list the total background rates in the detectors, as well as other detector characteristics required for the likelihood calculation [1][2][3][4][5][6]49,50]. In Table III we list the ǫ i , σ i , and B i values for each event reported in each detector.…”

Section: The Reported Datamentioning

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: The Reported Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Bayesian analysis of neutrinos observed from supernova SN 1987A

2002

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“…The neutrino observations of supernova (SN) 1987A [1][2][3][4][5][6] have long been taken as a confirmation of the salient features of our physical understanding of the corecollapse SN phenomenon. At the same time, a detailed interpretation [7][8][9][10][11][12][13][14] of the data is difficult because of a number of "anomalies" [15].…”

Section: Introductionmentioning

confidence: 99%

Analysis of the SN 1987A neutrinos with a flexible spectral shape

Mirizzi

Raffelt

2005

Phys. Rev. D

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We analyze the neutrino events from the supernova (SN) 1987A detected by the Kamiokande II (KII) and Irvine-Michigan-Brookhaven (IMB) experiments. For the time-integrated flux we assume a quasi-thermal spectrum of the form (E/E0) α e −(α+1)E/E 0 where α plays the role of a spectral index. This simple representation not only allows one to fit the total energy Etot emitted inνe and the average energy Eν e , but also accommodates a wide range of shapes, notably anti-pinched spectra that are broader than a thermal distribution. We find that the pile-up of low-energy events near threshold in KII forces the best-fit value for α to the lowest value of any assumed prior range. This applies to the KII events alone as well as to a common analysis of the two data sets. The preference of the data for an "unphysical" spectral shape implies that one can extract meaningful values for Eν e and Etot only if one fixes a prior value for α. The tension between the KII and IMB data sets and theoretical expectations for Eν e is not resolved by an anti-pinched spectrum.PACS numbers: 14.60. Pq, 95.55.Vj, 95.85.Ry, 97.60.Bw

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“…Very crudely the above picture was already confirmed by the observation of the 1987a SN neutrinos. Clearly, the details of the observed spectra shows some puzzling features [31,32,33,34] which call for more data. We expect that in the future substantial theoretical and experimental progress will be made 5 to further improve the understanding of the emitted neutrino spectra.…”

Section: A Present Knowledge Of the Sn Ratementioning

confidence: 99%

Probing Dark Energy via Neutrino and Supernova Observatories

Hall¹,

Murayama²,

Papucci³

et al. 2006

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A novel method for extracting cosmological evolution parameters is proposed, using a probe other than light: future observations of the diffuse anti-neutrino flux emitted from core-collapse supernovae (SNe), combined with the SN rate extracted from future SN surveys. The relic SN neutrino differential flux can be extracted by using future neutrino detectors such as Gadoliniumenriched, megaton, water detectors or 100-kiloton detectors of liquid Argon or liquid scintillator.The core-collapse SN rate can be reconstructed from direct observation of SN explosions using future precision observatories. Our method, by itself, cannot compete with the accuracy of the optical-based measurements but may serve as an important consistency check as well as a source of complementary information. The proposal does not require construction of a dedicated experiment, but rather relies on future experiments proposed for other purposes.

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Angular distribution of events from SN1987A

Cited by 151 publications

References 2 publications

Bayesian analysis of neutrinos observed from supernova SN 1987A

Bayesian analysis of neutrinos observed from supernova SN 1987A

Analysis of the SN 1987A neutrinos with a flexible spectral shape

Probing Dark Energy via Neutrino and Supernova Observatories

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