Diffuse neutrino supernova background as a cosmological test

Barranco, J.; Bernal, Argelia; Delépine, D.

doi:10.1088/1361-6471/aab8ae

Cited by 9 publications

(4 citation statements)

References 50 publications

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“…For recent studies of the impact of different cosmological models on the DSNB, the reader is referred to Barranco et al (2018) or Yang et al (2019). Having described our computational model with all of its required inputs, we now proceed to the discussion of our results.…”

Section: Cosmological Modelmentioning

confidence: 99%

Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background

Kresse,

Ertl,

Janka

2020

Preprint

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The diffuse cosmic supernova neutrino background (DSNB) is observational target of the gadoliniumloaded Super-Kamiokande (SK) detector and the forthcoming JUNO and Hyper-Kamiokande detectors. Current predictions are hampered by our still incomplete understanding of the supernova (SN) explosion mechanism and of the neutron star (NS) equation of state and maximum mass. In our comprehensive study we revisit this problem on grounds of the landscapes of successful and failed SN explosions obtained by Sukhbold et al. and Ertl et al. with parametrized one-dimensional neutrino engines for large sets of single-star and helium-star progenitors, with the latter serving as proxy of binary evolution effects. Besides considering engines of different strengths, leading to different fractions of failed SNe with black-hole (BH) formation, we also vary the NS mass limit, the spectral shape of the neutrino emission, and include contributions from poorly understood alternative NS-formation channels such as accretion-induced or merger-induced collapse events. Since the neutrino signals of our large model sets are approximate, we calibrate the associated degrees of freedom by using state-of-the-art simulations of proto-neutron star cooling. Our predictions are higher than other recent ones because of a large fraction of failed SNe with long delay to BH formation. Our best-guess model predicts a DSNB νe -flux of 28.8 +24.6 −10.9 cm −2 s −1 with 6.0 +5.1 −2.1 cm −2 s −1 in the favorable measurement interval of [10,30] MeV, and 1.3 +1.1 −0.4 cm −2 s −1 with νe energies > 17.3 MeV, which is roughly a factor of two below the current SK limit. The uncertainty range is dominated by the still insufficiently constrained cosmic rate of stellar core-collapse events.

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Section: Cosmological Modelmentioning

confidence: 99%

Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background

Kresse,

Ertl,

Janka

2020

Preprint

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“…By using the DSNB data, one can test the standard $CDM model including the measurement of the Hubble constant 109) or other exotic models such as a logotropic universe and a bulk viscous matter-dominated universe. 111) 4.4. Core collapse to black holes.…”

Section: Neutrino Spectrum Of Various Flavorsmentioning

confidence: 99%

Diffuse neutrino background from past core collapse supernovae

ANDO,

EKANGER,

HORIUCHI

et al. 2023

Proceedings of the Japan Academy. Ser. B: Physical and Biologic

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Core collapse supernovae are among the most powerful explosions in the Universe, which emit thermal neutrinos that carry away most of the gravitational binding energy released. These neutrinos produce a diffuse supernova neutrino background (DSNB), which is one of the largest energy budgets among all radiation backgrounds. Detecting the DSNB is an important goal of modern high-energy astrophysics and particle physics, which provides valuable insights into core collapse modeling, neutrino physics, and cosmic supernova rate history. In this review, the key ingredients of DSNB calculation and what can be learned from future detections, including black hole formation and non-standard neutrino interactions are discussed. Moreover, an overview of the latest updates in neutrino experiments, which could lead to the detection of the DSNB in the next decade, is provided. With the promise of this breakthrough discovery on the horizon, the study of DSNB has great potential to further our understanding of the Universe.

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“…The diffuse supernova neutrino background (DSNB) is also of interest as an astrophysical target [65,[187][188][189]. A measurement of the DSNB flux would be an independent probe of cosmology, as well as representing an average of supernova bursts.…”

Section: Supernovaementioning

confidence: 99%

CYGNUS: Feasibility of a nuclear recoil observatory with directional sensitivity to dark matter and neutrinos

Vahsen¹,

O’Hare²,

Lynch³

et al. 2020

Preprint

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Now that conventional weakly interacting massive particle (WIMP) dark matter searches are approaching the neutrino floor, there has been a resurgence of interest in detectors with sensitivity to nuclear recoil directions. A large-scale directional detector is attractive in that it would have sensitivity below the neutrino floor, be capable of unambiguously establishing the galactic origin of a purported dark matter signal, and could serve a dual purpose as a neutrino observatory. We present the first detailed analysis of a 1000 m 3 -scale detector capable of measuring a directional nuclear recoil signal at low energies. We propose a modular and multi-site observatory consisting of time projection chambers (TPCs) filled with helium and SF6 at atmospheric pressure. By comparing several available readout technologies, we identify high-resolution strip readout TPCs as the optimal tradeoff between performance and cost. We estimate that suitable angular resolution and head-tail recognition is achievable down to helium recoil energies of ∼6 keVr. Depending on the readout technology, an average of only 4-5 detected 100-GeV c −2 WIMP-fluorine recoils above 50 keVr are sufficient to rule out an isotropic recoil distribution at 90% CL. An average of 10-20 helium recoils above 6 keVr or only 3-4 helium recoils above 20 keVr would suffice to distinguish a 10 GeV c −2 WIMP signal from the solar neutrino background. High-resolution TPC charge readout also enables powerful electron background rejection capabilities well below 10 keV. We detail background and site requirements at the 1000 m 3 -scale, and identify materials that require improved radiopurity. The final experiment, which we name Cygnus-1000, will be able to observe ∼ 10-40 neutrinos from the Sun, depending on the final energy threshold. With the same exposure, the sensitivity to spin independent cross sections will extend into presently unexplored sub-10 GeV c −2 parameter space. For spin dependent interactions, already a 10 m 3 -scale experiment could compete with upcoming generation-two detectors, but Cygnus-1000 would improve upon this considerably. Larger volumes would bring sensitivity to neutrinos from an even wider range of sources, including galactic supernovae, nuclear reactors, and geological processes.

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Diffuse neutrino supernova background as a cosmological test

Cited by 9 publications

References 50 publications

Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background

Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background

Diffuse neutrino background from past core collapse supernovae

CYGNUS: Feasibility of a nuclear recoil observatory with directional sensitivity to dark matter and neutrinos

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