On the Event Observed in the Mont Blanc Underground Neutrino Observatory during the Occurrence of Supernova 1987
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Aglietta, M.; Badino, G.; Bologna, G.; Castagnoli, C.; Castellina, A.; Dadykin, V. L.; Fulgione, W.; Galeotti, P.; Kalchukov, F. F.; Kortchaguin, B.; Kortchaguin, P. V.; Malguin, A. S.; Ryassny, V. G.; Ryazhskaya, O. G.; Saavedra, O.; Talochkin, V. P.; Trinchero, G.; Vernetto, S.; Зацепин, Г. Т.; Yakushev, V. F.

doi:10.1209/0295-5075/3/12/011

Cited by 216 publications

(100 citation statements)

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“…Nevertheless, strong theoretical evidence exists for the existence of a neutron star in SNR 1987A from detailed studies of the progenitor [e.g. 31,32], and the coincident worldwide detection of core collapse neutrinos from the supernova event [33][34][35][36]. Although no pulsar detection has been confirmed, numerous searches have placed upper limits on the flux and luminosity at radio [ [39] reported finding an optical pulsar in SNR 1987A with a frequency of 467.5 Hz, modulated sinusoidally with a ∼ 1-ks period, consistent with precession given an ellipticity of ∼ 10 −6 .…”

Section: A Neutron Star In Snr 1987a?mentioning

confidence: 99%

Cross-correlation search for continuous gravitational waves from a compact object in SNR 1987A in LIGO Science run 5

et al. 2016

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We present the results of a cross-correlation search for gravitational waves from SNR 1987A using the second year of LIGO Science Run 5 data. The frequency band 75-450 Hz is searched. No evidence of gravitational waves is found. A 90% confidence upper limit of h0 ≤ 3.8 × 10 −25 is placed on the gravitational wave strain at the most sensitive frequency near 150 Hz. This corresponds to an ellipticity of ≤ 8.2 × 10 −4 and improves on previously published strain upper limits by a factor ≈ 4. We perform a comprehensive suite of validations of the search algorithm and identify several computational savings which marginally sacrifice sensitivity in order to streamline the parameter space being searched. We estimate detection thresholds and sensitivities through Monte-Carlo simulations.PACS numbers: 95.85.Sz, 97.60.Jd

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Section: A Neutron Star In Snr 1987a?mentioning

confidence: 99%

Cross-correlation search for continuous gravitational waves from a compact object in SNR 1987A in LIGO Science run 5

et al. 2016

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“…On February 23, 1987, several experiments [1,2,3,4] contributed to begin the era of extragalactic neutrino astronomy. These observations had an enormous impact on astrophysics and on particle physics.…”

Section: Motivation and Contextmentioning

confidence: 99%

Is there a problem with low energy SN1987A neutrinos?

Costantini¹,

Ianni²,

Pagliaroli³

et al. 2007

J. Cosmol. Astropart. Phys.

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The observation of several low energy events during the SN1987A burst made by Kamiokande-II is somewhat puzzling when compared with the theoretical expectations and with the observations of IMB, and has an important weight in the attempts to use these data to learn about the properties of the supernova neutrinos. In this paper, we analyze the possibility that a few of the 12 events observed by Kamiokande-II (or 11, neglecting the event number 6) are due to background. The volume distribution of these events is not a uniform distribution at the 3 σ level and this suggests the presence of background events close or at the border of the volume used for the analysis. The theoretical energy distribution is not in perfect agreement with the observations, but the disagreement is not severe, especially when we consider the presence of a peak of low energy background events. The expected energy distribution is used to show that the observation of a supernova neutrino signal has a significance of 8.5 σ and that 2 − 4 background events are plausible. In summary, the distributions of the events in space and in energy support the hypothesis that 3 or 4 of the low energy events-a priori, 2.3 of them-are due to background.In this way, we can argue that there is no actual disagreement between the average energy of the supernova neutrinos seen in Kamiokande-II and the theoretical expectations, the remaining discrepancy being a 1 σ effect. PACS

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“…That day at about 2:52 UT LSD detector [26] and at about 7:35 UT BUST [27], KII (Japan-USA, Kamioka) [28] and IMB (USA, Cleveland) [29] detectors measured neutrino radiation from collapsing star for the first time in the history of science. The burst was very distant, at a distance of 50 kpc.…”

Section: A Supernovae Explosion Sn1987amentioning

confidence: 99%

Study of the penetrating component of cosmic rays underground using large scintillation detectors

Ryazhskaya

2016

J. Phys.: Conf. Ser.

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Abstract. The study of penetrating component of cosmic ray underground using large scintillation detectors situated in Russia and Italy is carried out during more than 40 years. The main results obtained at the different depths from 25 m w.e. to 5200 m w.e. are presented in this report. IntroductionThe term "Underground Physics" was introduced by prof. C. Castagnoli during the 1 st symposium on Underground physics in Saint-Vincent (UP-85) dedicated to the opening ceremony of the russianitalian LSD detector under MontBlanc [1]. In this year we can celebrate 30 years of Underground Physics (UP). UP as physics in general is the experimental science. The mother of the truth in physics is the experiment. Therefore paying tribute to the wonderful works of theoreticians in this field of knowledge we will say here about the experiments carried out by collaborators of Russian Academy of Science and collaborators of RAS with their Italian colleagues in UP during that time: ASD (Arteomovsk Scintillation Detector) [2], BUST (Baksan Underground Scintillation Telescope) [3], LSD (Liquid Scintillation Detector) [4,5], LVD (Large Volume Detector) [6,7], SAGE (Ga-Ge experiment for solar neutrino detection in Baksan) [8], Baikal underwater experiment [9].The main problems of UP are: 1. Study of neutrino radiation (atmospheric neutrinos; solar neutrinos; neutrinos from collapsing stars); 2. Construction of underground detectors; 3. Detection of neutrino radiation from SN1987A; 4. Study of penetrating component of cosmic rays (energy spectrum; study of deep inelastic scattering of muons; generation of nuclear active component underground; depth-intensity curve of muons; depth-intensity curve of neutrons; seasonal modulation of the cosmic ray muon flux and neutron flux from muons; μ+/μ-ratio).

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On the Event Observed in the Mont Blanc Underground Neutrino Observatory during the Occurrence of Supernova 1987 a

Abstract: A. S. 1)6Au=uIN(), V. G. RYASSNY(), 0. G. RYAZHSKAYA(**), 0. SAAVEDRA(*), V. P. TALQCHEIN(**), G. TRINCHERO(), S. VERNE~TO(), G. T. ZATSEPIN() and V. F. YAKUSHEV() (*) Istituto di C o s m o g w f e del C.N.R.

Cited by 216 publications

References 4 publications

Cross-correlation search for continuous gravitational waves from a compact object in SNR 1987A in LIGO Science run 5

Cross-correlation search for continuous gravitational waves from a compact object in SNR 1987A in LIGO Science run 5

Is there a problem with low energy SN1987A neutrinos?

Study of the penetrating component of cosmic rays underground using large scintillation detectors

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On the Event Observed in the Mont Blanc Underground Neutrino Observatory during the Occurrence of Supernova 1987 a

Abstract: A. S. 1)6Au=uIN(**), V. G. RYASSNY(**), 0. G. RYAZHSKAYA(**), 0. SAAVEDRA(*), V. P. TALQCHEIN(**), G. TRINCHERO(*), S. VERNE~TO(*), G. T. ZATSEPIN(**) and V. F. YAKUSHEV(**) (*) Istituto di C o s m o g w f e del C.N.R.

Cited by 216 publications

References 4 publications

Cross-correlation search for continuous gravitational waves from a compact object in SNR 1987A in LIGO Science run 5

Cross-correlation search for continuous gravitational waves from a compact object in SNR 1987A in LIGO Science run 5

Is there a problem with low energy SN1987A neutrinos?

Study of the penetrating component of cosmic rays underground using large scintillation detectors

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Product

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Abstract: A. S. 1)6Au=uIN(), V. G. RYASSNY(), 0. G. RYAZHSKAYA(**), 0. SAAVEDRA(*), V. P. TALQCHEIN(**), G. TRINCHERO(), S. VERNE~TO(), G. T. ZATSEPIN() and V. F. YAKUSHEV() (*) Istituto di C o s m o g w f e del C.N.R.