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Arrival directions of neutrino events from IceCube. Shown are upgoing track events [8,9] (), the high-energy starting events (HESE) (tracks ⊗ and cascades ⊕) [6, 7, 10], and additional track events published as public alerts () [23, 24]. The blue-shaded region indicates where the Earth absorption of 100-TeV neutrinos becomes important. The dashed line indicates the equatorial plane. We also indicate the location of the blazar TXS 0506+056 ().
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I am not an author, but one of the Endorsers. This is a remarkable and interesting proposal and needs to be spread.
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... last decade ushered in high-energy neutrino astronomy, with the discovery of an astrophysical neutrino flux in the 10 TeV -10 PeV energy range [4][5][6][7][8][9][10]. The arrival directions of the most energetic neutrinos are shown in Fig. 1 and are consistent with a uniform distribution across the sky after accounting for detector acceptance. Neutrino emission at the observed flux level has been predicted from a variety of source classes, including γ-ray bursts, blazars, starburst galaxies, galaxy clusters, and others (see, e.g. [13,14]). Recently, coincident observations ...
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... The recent observations of neutrinos from blazar TXS 0506+056 coincident with γ-rays provide the first evidence of an extragalactic neutrino source [8,9]. As articulated in the Astro 2020 science white paper "Astrophysics Uniquely Enabled by Observations of High-Energy Cosmic Neutrinos" [10], neutrinos carry unique information about the most energetic non-thermal sources in the universe. The concept presented here is designed to extend observations of neutrinos to higher energies, covering the range of 1-100 PeV, with tau neutrinos (ν τ ) in response to the strategy advocated by the neutrino astrophysics community [10] of a multi-observatory approach that would extend the science reach of neutrino observatories. ...
... As articulated in the Astro 2020 science white paper "Astrophysics Uniquely Enabled by Observations of High-Energy Cosmic Neutrinos" [10], neutrinos carry unique information about the most energetic non-thermal sources in the universe. The concept presented here is designed to extend observations of neutrinos to higher energies, covering the range of 1-100 PeV, with tau neutrinos (ν τ ) in response to the strategy advocated by the neutrino astrophysics community [10] of a multi-observatory approach that would extend the science reach of neutrino observatories. ...
... The sources are expected to produce primarily electron (ν e ) and muon (ν µ ) neutrinos with the ν τ component resulting only from neutrino flavor conversion during propagation over astronomical distances. Characterization of the ν τ component of the astrophysical neutrino flux, in combination with the observations of IceCube and other detectors such as KM3NeT, are key observables to constrain the neutrino production mechanisms and physical conditions at the sources [10,17,18] as well as new neutrino physics [19][20][21][22][23]. ...
High-energy astrophysical neutrinos, recently discovered by IceCube up to energies of several PeV, opened a new window to the high-energy Universe. Yet much remains to be known. IceCube has excellent muon flavor identification, but tau flavor identification is challenging. This limits its ability to probe neutrino physics and astrophysics. To address this limitation, we present a concept for a large-scale observatory of astrophysical tau neutrinos in the 1-100 PeV range, where a flux is guaranteed to exist. Its detection would allow us to characterize the neutrino sources observed by IceCube, to discover new ones, and test neutrino physics at high energies. The deep-valley air-shower array concept that we present provides highly background-suppressed neutrino detection with pointing resolution <1 degree, allowing us to begin the era of high-energy tau-neutrino astronomy.
... High-energy neutrino astronomy is a most promising approach to address the still unanswered question of the origin of high-energy cosmic rays [1]. Neutrinos are the perfect messenger. ...
... A two orders of magnitude increase in the volume instrumented by IceCube is considered costprohibitive due to the attenuation and scattering of optical light in ice [5]. Such a detector may measure the continuation of the neutrino flux, as well as the expected fluxes in the ultra-high energy regime [1]. ...
... The ARIANNA project [8,9] uses an array of autonomous detector stations with antennas located close to the ice surface, whereas the ARA project [10] uses antennas at a depth of up to 200 m below the firn layer. The experimental techniques matured substantially over the last years [11,12] and the community is well prepared for the construction of a large scale Askaryan detector with enough exposure to measure the continuation of the astrophysical neutrino flux to higher energies [1], to potentially discover cosmogenic neutrinos [13][14][15], and measure particle physics properties at yet unachieved energies [16]. ...
NuRadioMC is a Monte Carlo framework designed to simulate ultra-high energy neutrino detectors that rely on the radio detection method. This method exploits the radio emission generated in the electromagnetic component of a particle shower following a neutrino interaction. NuRadioMC simulates everything from the neutrino interaction in a medium, the subsequent Askaryan radio emission, the propagation of the radio signal to the detector and finally the detector response. NuRadioMC is designed as a modern, modular Python-based framework, combining flexibility in detector design with user-friendliness. It includes a state-of-the-art event generator, an improved modelling of the radio emission, a revisited approach to signal propagation and increased flexibility and precision in the detector simulation. This paper focuses on the implemented physics processes and their implications for detector design. A variety of models and parameterizations for the radio emission of neutrino-induced showers are compared and reviewed. Comprehensive examples are used to discuss the capabilities of the code and different aspects of instrumental design decisions.
... Very high-energy cosmic neutrinos are emitted in a number of models of astrophysical transient events [27,28]. Astrophysical sources generally produce electron and muon neutrinos, which after astronomical propagation distances, arrive on Earth with approximately equal numbers of the three flavors: electron, muon, and tau neutrinos. ...
The Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) is a NASA Astrophysics probe-class mission designed to observe ultra-high energy cosmic rays (UHECRs) and cosmic neutrinos from space. Astro2020 APC white paper: Medium-class Space Particle Astrophysics Project.
... At the EeV scale, cosmogenic neutrinos, produced by UHE cosmic rays interacting with photon backgrounds through the GZK effect [17,18], are predicted but have not yet been observed [19][20][21]. See Ref. [22] for a discussion of astrophysics enabled by observations of cosmic neutrinos. ...
High-energy cosmic neutrinos can reveal new fundamental particles and interactions, probing energy and distance scales far exceeding those accessible in the laboratory. This white paper describes the outstanding particle physics questions that high-energy cosmic neutrinos can address in the coming decade. A companion white paper discusses how the observation of cosmic neutrinos can address open questions in astrophysics. Tests of fundamental physics using high-energy cosmic neutrinos will be enabled by detailed measurements of their energy spectrum, arrival directions, flavor composition, and timing.
The end state of binary-neutron-star (BNS) mergers can manifest conditions to produce high-energy neutrinos. Inspired by the event GW170817, detected in gravitational waves and in optical/infrared emission, we investigate a scenario in which cosmic-ray (CR) particles are accelerated, in a population of BNS mergers, in the energy range that might contribute from the knee to the ankle of the CR measured spectrum. By taking into account the measured thermal and non-thermal energy density of the photon fields in the source environment as a function of the time after the merger, we model the CR interactions and the consequent neutrino production. We propagate the escaped CR and neutrino fluxes through the extragalactic space and compare the expected diffuse fluxes to the experimental data and current limits. Depending on the CR spectral and composition parameters at acceleration, and on the possible contribution to the sub-ankle CR flux, we discuss the predicted diffuse neutrino flux associated to this class of astrophysical objects, as a function of the details of the photon field characterizing the merger stage, including its evolution in time. We constrain the fraction of accelerated baryons in the source site given the BNS merger rate per volume, taking into account at the same time the constraints from the measured CR and neutrino fluxes.
SND@LHC is a compact and stand-alone experiment designed to perform measurements with neutrinos produced at the LHC in the pseudo-rapidity region of 7.2 < η < 8.4. The experiment is located 480 m downstream of the ATLAS interaction point, in the TI18 tunnel. The detector is composed of a hybrid system based on an 830 kg target made of tungsten plates, interleaved with emulsion and electronic trackers, also acting as an electromagnetic calorimeter, and followed by a hadronic calorimeter and a muon identification system. The detector is able to distinguish interactions of all three neutrino flavours, which allows probing the physics of heavy flavour production at the LHC in the very forward region. This region is of particular interest for future circular colliders and for very high energy astrophysical neutrino experiments. The detector is also able to search for the scattering of Feebly Interacting Particles. In its first phase, the detector is ready to operate throughout LHC Run 3 and collect a total of 250 fb ⁻¹ .
The origin of high-energy cosmic rays, and their behavior in astrophysical sources, remains an open question. Recently, new ways to address this question have been made possible by the observation of a new astrophysical messenger, namely neutrinos. The IceCube telescope has detected a diffuse flux of astrophysical neutrinos in the TeV-PeV energy range, likely produced in astrophysical sources accelerating cosmic rays, and more recently it has reported on a few candidate individual neutrino sources. Future experiments will be able to improve on these measurements quantitatively, by the detection of more events, and qualitatively, by extending the measurement into the EeV energy range. In this paper, we review the main features of the neutrino emission and sources observed by IceCube, as well as the main candidate sources that could contribute to the diffuse neutrino flux. As a parallel question, we review the status of high-energy neutrinos as a probe of Beyond the Standard Model physics coupling to the neutrino sector.
The tRopIcal DEep-sea Neutrino Telescope (TRIDENT) is a future large-scale next-generation neutrino telescope. In September 2021, the TRIDENT pathfinder experiment (TRIDENT EXplorer, T-REX for short) completed
in-situ
measurements of deep-sea water properties in the South China Sea. The T-REX apparatus integrates two independent and complementary systems, a photomultiplier tube and a camera system, to measure the optical and radioactive properties of the deep-sea water. One light emitter module and two light receiver modules were deployed, which were synchronized by using White Rabbit technology. The light emitter module generates nanosecond-width light-emitting diode pulses, while the light receiver module hosts three photomultiplier tubes and a camera to detect photons. The submerged apparatus and the data acquisition system perform real-time command and data transmission. We report the design and performance of the readout electronics for T-REX, including hardware modules, firmware design for digital signal processing, and host-computer software.
Upcoming neutrino telescopes may discover ultra-high-energy (UHE) cosmic neutrinos, with energies beyond 100 PeV, in the next 10–20 years. Finding their sources would identify guaranteed sites of interaction of UHE cosmic rays, whose origin is unknown. We search for sources by looking for multiplets of UHE neutrinos arriving from similar directions. Our forecasts are state-of-the-art, geared at neutrino radio-detection in IceCube-Gen2. They account for detector energy and angular response, and for critical, but uncertain backgrounds. Sources at declination of -45° to 0° will be easiest to discover. Discovering even one steady-state source in 10 years would imply that the source has an UHE neutrino luminosity at least larger than about 10 ⁴³ erg/s (depending on the source redshift evolution). Discovering no transient source would disfavor transient sources brighter than 10 ⁵³ erg as dominant. Our results aim to inform the design of upcoming detectors.
Sensitivity to ultra-high-energy neutrinos ( E > 17 eV) can be obtained cost-efficiently by exploiting the Askaryan effect in ice, where a particle cascade induced by the neutrino interaction produces coherent radio emission that can be picked up by antennas. As the near-surface ice properties change rapidly within the upper 𝒪(100 m), a good understanding of the ice properties is required to reconstruct the neutrino properties. In particular, continuous monitoring of the snow accumulation (which changes the depth of the antennas) and the index-of-refraction n ( z ) profile are crucial for an accurate determination of the neutrino's direction and energy. We present an in-situ calibration system that extends the radio detector station with two radio emitters to continuously monitor the firn properties within the upper 40 m by measuring the time differences between direct and reflected (off the surface) signals (D'n'R). We determine the optimal positions of two transmitters at all three sites of current and future in-ice radio detectors: Greenland, Moore's Bay, and the South Pole. For the South Pole we find that the snow accumulation Δ h can be measured with a resolution of 3 mm and the parameters of an exponential n ( z ) profile α and z 0 with 0.04% and 0.14% precision respectively, which constitutes an improvement of more than a factor of 10 as compared to the inference of the n ( z ) profile from density measurements. Additionally, as this technique is based on the measurement of the signal propagation times we are not bound to the conversion of density to index-of-refraction. We quantify the impact of these ice uncertainties on the reconstruction of the neutrino vertex, direction, and energy and find that the calibration device measures the ice properties to sufficient precision to have negligible influence.