Impact of binary interactions on the diffuse supernova neutrino background

Horiuchi, Shunsaku; Kinugawa, Tomoya; Takiwaki, Tomoya; Takahashi, Koh; Kotake, Kei

doi:10.1103/physrevd.103.043003

Cited by 44 publications

(34 citation statements)

References 134 publications

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“…shown only for the signal window. Right: upper limits on the extraterrestrial electron antineutrino flux from the present work, in comparison with previous published results from SK [1,2] and KamLAND [7] and theoretical predictions from Refs [2,[8][9][10][11][12][13] (in gray).…”

Section: Pos(icrc2021)1139supporting

confidence: 60%

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Diffuse Supernova Neutrino Background Search at Super-Kamiokande

Hedri¹,

Ashida²,

Giampaolo³

2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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We present the results of a search for the Diffuse Supernova Neutrino Background (DSNB) at Super-Kamiokande (SK) that incorporates 22.5 × 2970 kton.days of data from its fourth datataking phase. Two analyses, with different energy regimes covering the 9.3−81.3 MeV antineutrino energy range, have been developed based on previous SK searches, with substantially improved background modeling and data reduction techniques. Moreover, a combined analysis of nearly 20 years of SK data has been performed, with a 90% C.L. sensitivity to the DSNB flux comparable to various DSNB predictions. No significant evidence for a DSNB signal has been observed, and both analyses set world-leading limits on the DSNB flux that can reach about 2.7 .cm −2 .s −1 for a wide range of models.

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Section: Pos(icrc2021)1139supporting

confidence: 60%

“…Figure 4: Left: 90% confidence limits on the DSNB flux, best-fit fluxes, and sensitivities for the combined SK analysis for a range of DSNB models[2,[8][9][10][11][12][13]. Also shown are the limits from the previous analysis from Ref [1].…”

mentioning

confidence: 99%

Diffuse Supernova Neutrino Background Search at Super-Kamiokande

Hedri¹,

Ashida²,

Giampaolo³

2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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“…• The possibility of compact objects that are bright in X-ray or neutrino emission may allow the detection of these objects individually, or more probably, through their additional contributions to the diffuse supernova neutrino background, which may soon be detected at Super-K [472]. This effect has also been suggested from considerations of binary-star interactions [473].…”

Section: Discussionmentioning

confidence: 99%

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

Berryman,

Gardner,

Zakeri

2022

Preprint

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The neutron lifetime anomaly has been used to motivate the introduction of new physics with hidden-sector particles coupled to baryon number, and on which neutron stars provide powerful constraints. Although the neutron lifetime anomaly may eventually prove to be of mundane origin, we use it as motivation for a broader review of the ways that baryon number violation, be it real or apparent, and dark sectors can intertwine and how neutron star observables, both present and future, can constrain them.

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“…Here we carry out the DSNB modeling simply; for overviews tackling the astrophysical uncertainties affecting the signal, see Refs. [82][83][84][85][86]. Following Ref.…”

Section: A Calculation Of the Dsnb Signalmentioning

confidence: 99%

Towards Probing the Diffuse Supernova Neutrino Background in All Flavors

Suliga,

Beacom,

Tamborra

2021

Preprint

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Fully understanding the average core-collapse supernova requires detecting the diffuse supernova neutrino background (DSNB) in all flavors. While the DSNB νe flux is near detection, and the DSNB νe flux has a good upper limit and promising prospects for improved sensitivity, the DSNB νx (each of νµ, ντ , νµ, ντ ) flux has a poor limit and heretofore had no clear path for improved sensitivity. We show that a succession of xenon-based dark matter detectors -XENON1T (completed), XENONnT (under construction), and DARWIN (proposed) -can dramatically improve sensitivity to DSNB νx the neutrino-nucleus coherent scattering channel. XENON1T could match the present sensitivity of ∼ 10 3 cm −2 s −1 per νx flavor, XENONnT would have linear improvement of sensitivity with exposure, and a long run of DARWIN could reach a flux sensitivity of ∼ 10 cm −2 s −1 . Together, these would also contribute to greatly improve bounds on non-standard scenarios. Ultimately, to reach the standard flux range of ∼ 1 cm −2 s −1 , even larger exposures will be needed, which we show may be possible with the series of proposed lead-based RES-NOVA detectors.

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Impact of binary interactions on the diffuse supernova neutrino background

Cited by 44 publications

References 134 publications

Diffuse Supernova Neutrino Background Search at Super-Kamiokande

Diffuse Supernova Neutrino Background Search at Super-Kamiokande

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

Towards Probing the Diffuse Supernova Neutrino Background in All Flavors

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