Analytical assessment of the Beckman Coulter Unicel DxI AccuTnI+3 immunoassay

Lippi, Giuseppe; Dipalo, Mariella; Avanzini, Paola; Formentini, Alessandro; Aloe, Rosalia

doi:10.1515/dx-2013-0039

Cited by 21 publications

(17 citation statements)

References 1 publication

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“…In this equation, θ Ã is the zenith angle where the neutrinos are produced, taking account of the curvature of the Earth [33]. The parameters Φ 0 , A and B are free fit parameters, the spectral index is γ ¼ 2.7, and the critical energies are ϵ π ¼ 115 GeV and ϵ K ¼ 850 GeV.…”

Section: Fig 1 (Color Online)mentioning

confidence: 99%

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2014

Phys. Rev. D

102

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when the array was running in its 59-string configuration. The data sample was optimized to contain muon neutrino induced events with a background contamination of atmospheric muons of less than 1%. These data, which are dominated by atmospheric neutrinos, are analyzed with a global likelihood fit to search for possible contributions of prompt atmospheric and astrophysical neutrinos, neither of which have yet been identified. Such signals are expected to follow a harder energy spectrum than conventional atmospheric neutrinos. In addition, the zenith angle distribution differs for astrophysical and atmospheric signals. A global fit of the reconstructed energies and directions of observed events is performed, including possible neutrino flux contributions for an astrophysical signal and atmospheric backgrounds as well as systematic uncertainties of the experiment and theoretical predictions. The best fit yields an astrophysical signal flux for ν μ þν μ of E 2 · ΦðEÞ ¼ 0.25 × 10 −8 GeV cm −2 s −1 sr −1 ,

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Section: Fig 1 (Color Online)mentioning

confidence: 99%

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2014

Phys. Rev. D

102

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“…[22]. We try to reconstruct a reasonable flux of parent particles from the active neutrino flux of Ref.…”

Section: Properties Of the Heavy Neutrinomentioning

confidence: 99%

Heavy neutrino search in accelerator-based experiments

Asaka

Eijima

Watanabe

2013

J. High Energ. Phys.

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We explore the feasibility of detecting heavy neutrinos by the existing facilities of neutrino experiments. A heavy neutrino in the mass range 1 MeV M N 500 MeV is produced by pion or kaon decay, and decays to charged particles which leave signals in neutrino detectors. Taking the T2K experiment as a typical example, we estimate the heavy neutrino flux produced in the neutrino beam line. Due to massive nature of the heavy neutrino, the spectrum of the heavy neutrino is significantly different from that of the ordinary neutrinos. While the ordinary neutrinos are emitted to various directions in the laboratory frame due to their tiny masses, the heavy neutrinos tend to be emitted to the forward directions and frequently hit the detector. The sensitivity for the mixing parameters is studied by evaluating the number of signal events in the near detector ND280. For the electron-type mixing, the sensitivity of T2K at 10 21 POT is found to be better than that of the previous experiment PS191, which has placed the most stringent bounds on the mixing parameters of the heavy neutrinos for 140 MeV M N 500 MeV. IntroductionIn the last few decades, neutrino oscillation experiments have conclusively shown that neutrinos are massive [1]. The minimal version of the Standard Model is thus to be extended to accommodate the neutrino masses. In many possible extension of the Standard Model, neutral heavy leptons are often predicted. In the seesaw mechanism [2] for example, the right-handed neutrinos are introduced and they weakly mix with the ordinary neutrinos after the electroweak symmetry breaking.For the masses of the heavy neutrinos, a wide range of possibilities has been discussed in literature. In the canonical picture of the seesaw mechanism, heavy neutrino masses are supposed to be around the grand unification scale. These super-heavy neutrinos can account for the baryon asymmetry of the universe by the leptogenesis [3]. Another possibility to account for the baryon asymmetry has been suggested in [4,5] and further studied in [6]. In this scenario, two quasi-degenerate heavy neutrinos of O(100) MeV −O(10) GeV play a crucial role in the early universe. Heavy neutrinos in the mass range ∼ 0.2 GeV could enhance the energy transport from the core to the stalled shock and favor the supernova explosion [7]. Heavy neutrinos with a few keV mass have also attracted much interests as a viable dark matter candidate [8] and an agent of the pulsar velocities [9].Remarkably, the dark matter and the baryon asymmetry due to keV and GeV heavy neutrinos can originate in a simple framework so called νMSM [10,5], which is an extension of the Standard Model with just three generations of the right-handed neutrinos.Besides the super-heavy range much larger than TeV, such heavy neutrinos can be tested in existing and forthcoming experiments due to lower threshold energies of production (for example, see Ref. [11,12] and references therein).In this paper, we focus on the heavy neutrinos produced by kaon decays. The previous neutrino exper...

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“…The process rates are defined in terms of interaction and decay lengths in units of X. More details about the equation and solutions can be found in [4,5].…”

Section: Matrix Cascade Equationsmentioning

confidence: 99%

Phenomenology of atmospheric neutrinos

Fedynitch

2016

EPJ Web of Conferences

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Abstract. The detection of astrophysical neutrinos, certainly a break-through result, introduced new experimental challenges and fundamental questions about acceleration mechanisms of cosmic rays. On one hand IceCube succeeded in finding an unambiguous proof for the existence of a diffuse astrophysical neutrino flux, on the other hand the precise determination of its spectral index and normalization requires a better knowledge about the atmospheric background at hundreds of TeV and PeV energies. Atmospheric neutrinos in this energy range originate mostly from decays of heavy-flavor mesons, which production in the phase space relevant for prompt leptons is uncertain. Current acceleratorbased experiments are limited by detector acceptance and not so much by the collision energy. This paper recaps phenomenological aspects of atmospheric leptons and calculation methods, linking recent progress in flux predictions with particle physics at colliders, in particular the Large Hadron Collider.

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Analytical assessment of the Beckman Coulter Unicel DxI AccuTnI+3 immunoassay

Cited by 21 publications

References 1 publication

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Heavy neutrino search in accelerator-based experiments

Phenomenology of atmospheric neutrinos

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