Neutrinos from SN1987a in the IMB detector

Haines, T. J.; Bratton, C. B.; Casper, D.; Ciocio, A.; Claus, R.; Crouch, M. F.; Dye, S. T.; Errede, S.; Gajewski, W.; Goldhaber, M.; 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.; Shumard, E.; Sinclair, D.; Sobel, H. W.; Sulak, L.; Svoboda, R.; Thornton, G.; Velde, J. C. van der

doi:10.1016/0168-9002(88)91097-2

Cited by 30 publications

(22 citation statements)

References 7 publications

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“…Models of Sk −69 • 202 indicated that it had an initial mass of ∼20 M (Hillebrandt et al 1987). The mass range of the progenitor is consistent with the formation of a neutron star (Thielemann & Arnett 1985), and thus with the neutrino events reported by the KamiokaNDE (Hirata et al 1987) and IMB (Bionta et al 1987;Haines et al 1988) detectors. Models by Crotts & Heathcote (2000) suggest a transition from red supergiant (RSG) into blue supergiant (BSG) to explain the hourglass nebula structure, which envelopes the SN with three nearlystationary rings (Blondin & Lundqvist, 1993;Chevalier & Dwarkadas 1995;Martin & Arnett 1995;Morris & Podsiadlowski 2007).…”

Section: Introductionsupporting

confidence: 71%

Spectral and Morphological Analysis of the Remnant of Supernova 1987a With Alma and Atca

Zanardo

Staveley‐Smith

Indebetouw

et al. 2014

ApJ

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We present a comprehensive spectral and morphological analysis of the remnant of Supernova (SN) 1987A with the Australia Telescope Compact Array (ATCA) and the Atacama Large Millimeter/submillimeter Array (ALMA). The non-thermal and thermal components of the radio emission are investigated in images from 94 to 672 GHz (λ 3.2 mm to 450 µm), with the assistance of a high-resolution 44 GHz synchrotron template from the ATCA, and a dust template from ALMA observations at 672 GHz. An analysis of the emission distribution over the equatorial ring in images from 44 to 345 GHz highlights a gradual decrease of the east-to-west asymmetry ratio with frequency. We attribute this to the shorter synchrotron lifetime at high frequencies. Across the transition from radio to far infrared, both the synchrotron/dust-subtracted images and the spectral energy distribution (SED) suggest additional emission beside the main synchrotron component (S ν ∝ ν −0.73 ) and the thermal component originating from dust grains at T ∼ 22 K. This excess could be due to free-free flux or emission from grains of colder dust. However, a second flat-spectrum synchrotron component appears to better fit the SED, implying that the emission could be attributed to a pulsar wind nebula (PWN). The residual emission is mainly localised west of the SN site, as the spectral analysis yields −0.4 α −0.1 across the western regions, with α ∼ 0 around the central region. If there is a PWN in the remnant interior, these data suggest that the pulsar may be offset westward from the SN position.

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Section: Introductionsupporting

confidence: 71%

Spectral and Morphological Analysis of the Remnant of Supernova 1987a With Alma and Atca

Zanardo

Staveley‐Smith

Indebetouw

et al. 2014

ApJ

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“…With this method, the uncertainty on the parameters estimation is given by the width of the distribution (RMS) of the difference between the fitted and the true values. The analysis is performed for three different hypotheses on the shape parameter and the signal scale: first assuming α and Λ are precisely known, second limiting the range to the true value ± 10% for both parameters, and third assuming Λ being free in the range [0, 2.5], and considering a physically allowed range for α being [2,4]. For the first case, the mean neutrino energy resolution is 0.25 MeV (∼ 2%).…”

Section: Estimation Of the Neutrino Spectrum Parametersmentioning

confidence: 99%

“…The first and only supernova neutrinos were observed from the SN 1987A explosion in the Large Magellanic Cloud. Two dozen events were detected by three neutrino detectors in operation at that time [3][4][5]. With the new generation of neutrino detectors, the observation of the next CCSN will provide invaluable insights into the astro-, subnuclear and nuclear physics involved in these extreme phenomena.…”

Section: Introductionmentioning

confidence: 99%

The KM3NeT potential for the next core-collapse supernova observation with neutrinos

et al. 2021

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The KM3NeT research infrastructure is under construction in the Mediterranean Sea. It consists of two water Cherenkov neutrino detectors, ARCA and ORCA, aimed at neutrino astrophysics and oscillation research, respectively. Instrumenting a large volume of sea water with $$\sim {6200}$$ ∼ 6200 optical modules comprising a total of $$\sim {200{,}000}$$ ∼ 200 , 000 photomultiplier tubes, KM3NeT will achieve sensitivity to $$\sim {10} \ \mathrm{MeV}$$ ∼ 10 MeV neutrinos from Galactic and near-Galactic core-collapse supernovae through the observation of coincident hits in photomultipliers above the background. In this paper, the sensitivity of KM3NeT to a supernova explosion is estimated from detailed analyses of background data from the first KM3NeT detection units and simulations of the neutrino signal. The KM3NeT observational horizon (for a $$5\,\sigma $$ 5 σ discovery) covers essentially the Milky-Way and for the most optimistic model, extends to the Small Magellanic Cloud ($$\sim {60} \ \mathrm{kpc}$$ ∼ 60 kpc ). Detailed studies of the time profile of the neutrino signal allow assessment of the KM3NeT capability to determine the arrival time of the neutrino burst with a few milliseconds precision for sources up to 5–8 kpc away, and detecting the peculiar signature of the standing accretion shock instability if the core-collapse supernova explosion happens closer than 3–5 kpc, depending on the progenitor mass. KM3NeT’s capability to measure the neutrino flux spectral parameters is also presented.

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“…99% of this energy is emitted as neutrinos, ∼1% goes into the kinetic energy associated with the external layers of the progenitor that are ejected at ∼10,000 km/s, and only 0.01% is radiated at UV, optical and near-infrared wavelengths. Therefore neutrinos are the ideal "messengers" for investigating the final stages of stellar evolution, even when the SN is not accessible to optical and radio telescopes [2][3][4][5]. Observations of a neutrino burst from SN 1987A have suggested that the formation of a neutron star might have occurred inside the SN remnant, nevertheless, this fact has been never unambiguously confirmed.…”

Section: Introductionmentioning

confidence: 99%

Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos

Agnes

Albergo

Albuquerque

et al. 2021

J. Cosmol. Astropart. Phys.

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Future liquid-argon DarkSide-20k and Argo detectors, designed for direct dark matter search, will be sensitive also to core-collapse supernova neutrinos, via coherent elastic neutrino-nucleus scattering. This interaction channel is flavor-insensitive with a high-cross section, enabling for a high-statistics neutrino detection with target masses of ∼50 t and ∼360 t for DarkSide-20k and Argo respectively. Thanks to the low-energy threshold of ∼0.5 keV nr achievable by exploiting the ionization channel, DarkSide-20k and Argo have the potential to discover supernova bursts throughout our galaxy and up to the Small Magellanic Cloud, respectively, assuming a 11-M progenitor star. We report also on the sensitivity to the neutronization burst, whose electron neutrino flux is suppressed by oscillations when detected via charged current and elastic scattering. Finally, the accuracies in the reconstruction of the average and total neutrino energy in the different phases of the supernova burst, as well as its time profile, are also discussed, taking into account the expected background and the detector response.

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Neutrinos from SN1987a in the IMB detector

Cited by 30 publications

References 7 publications

Spectral and Morphological Analysis of the Remnant of Supernova 1987a With Alma and Atca

Spectral and Morphological Analysis of the Remnant of Supernova 1987a With Alma and Atca

The KM3NeT potential for the next core-collapse supernova observation with neutrinos

Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos

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