scholarly journals Astronomy with energy dependent flavour ratios of extragalactic neutrinos

2021 ◽  
Vol 2021 (10) ◽  
Author(s):  
Siddhartha Karmakar ◽  
Sujata Pandey ◽  
Subhendu Rakshit
Keyword(s):  
Dark Matter ◽  
Energy Dependence ◽  
High Energy ◽  
Neutrino Energy ◽  
Density Profiles ◽  
Neutrino Telescopes ◽  
Astrophysical Neutrinos ◽  
Astrophysical Objects ◽  
Energy Dependent

Abstract High energy astrophysical neutrinos interacting with ultralight dark matter (DM) can undergo flavour oscillations that induce an energy dependence in the flavour ratios. Such a dependence on the neutrino energy will reflect in the track to shower ratio in neutrino telescopes like IceCube or KM3NeT. This opens up a possibility to study DM density profiles of astrophysical objects like AGN, GRB etc., which are the suspected sources of such neutrinos.

scholarly journals SEARCH FOR DARK MATTER WITH GAMMA-RAYS: A REVIEW

2013 ◽  
Vol 53 (A) ◽  
pp. 545-549 ◽  
Author(s):  
Aldo Morselli
Keyword(s):  
Dark Matter ◽  
Energy Range ◽  
Gamma Rays ◽  
Gamma Ray ◽  
High Energy ◽  
Space Telescope ◽  
High Energy Gamma ◽  
Astrophysical Objects ◽  
Energy Gamma

Successfully launched in June 2008, the Fermi Gamma-ray Space Telescope, formerly named GLAST, has been observing the high-energy gamma-ray sky with unprecedented sensitivity in<br />the 20MeV ÷ 300 GeV energy range and electrons + positrons in the 7 GeV ÷ 1TeV range, opening a new observational window on a wide variety of astrophysical objects.

scholarly journals High-energy neutrino interaction physics with IceCube

2019 ◽  
Vol 208 ◽  
pp. 09001
Author(s):  
Spencer Klein
Keyword(s):  
Standard Model ◽  
Cross Sections ◽  
Neutrino Flux ◽  
High Energy ◽  
Neutrino Interaction ◽  
Neutrino Telescopes ◽  
Neutrino Interactions ◽  
The Standard Model ◽  
Astrophysical Neutrinos ◽  
Neutrino Absorption

Although they are best known for studying astrophysical neutrinos, neutrino telescopes like IceCube can study neutrino interactions, at energies far above those that are accessible at accelerators. In this writeup, I present two IceCube analyses of neutrino interactions at energies far above 1 TeV. The first measures neutrino absorption in the Earth, and, from that determines the neutrino-nucleon cross-section at energies between 6.3 and 980 TeV. We find that the cross-sections are 1.30 +0.21 -0.19 (stat.) +0.39 -0.43 (syst.) times the Standard Model crosssection. We also present a measurement of neutrino inelasticity, using νμ charged-current interactions that occur within IceCube. We have measured the average inelasticity at energies from 1 TeV to above 100 TeV, and found that it is in agreement with the Standard Model expectations. We have also performed a series of fits to this track sample and a matching cascade sample, to probe aspects of the astrophysical neutrino flux, particularly the flavor ratio.

scholarly journals Ultra-high-energy cosmic rays from collisional annihilation revisited

2005 ◽  
Vol 83 (11) ◽  
pp. 1141-1149 ◽  
Author(s):  
R Dick ◽  
K M Hopp ◽  
K E Wunderle
Keyword(s):  
Dark Matter ◽  
Cosmic Rays ◽  
Cross Sections ◽  
Galactic Halo ◽  
High Energy ◽  
Source Distribution ◽  
Ultra High Energy ◽  
Density Profiles ◽  
High Energy Cosmic Rays ◽  
Dense Cores

We re-examine collisional annihilation of super-heavy dark-matter particles in dark-matter density spikes in the galactic halo as a possible source of ultra-high-energy cosmic rays. We estimate the possible flux in a way that does not depend on detailed assumptions about the density profiles of dark-matter clumps. The result confirms that collisional annihilation is compatible with annihilation cross sections below the unitarity bounds for super-heavy dark matter if the particles can form dense cores in the dark-matter substructure, and it provides estimates for core sizes and densities. The ensuing clumpy source distribution in the galactic halo will be tested within a few years of operation of the Pierre Auger observatory.PACS Nos.: 98.70.Sa, 98.70.–f, 95.35.+d, 14.80.–j

scholarly journals Lorentz Symmetry and High-Energy Neutrino Astronomy

Universe ◽  
2021 ◽  
Vol 7 (12) ◽  
pp. 490
Author(s):  
Carlos A. Argüelles ◽  
Teppei Katori
Keyword(s):  
Propagation Distance ◽  
High Energy ◽  
Lorentz Symmetry ◽  
Neutrino Energy ◽  
Research Field ◽  
Unique System ◽  
Mechanical Interference ◽  
Astrophysical Neutrinos ◽  
Neutrino Astronomy ◽  
Active Research

The search of the violation of Lorentz symmetry, or Lorentz violation (LV), is an active research field. The effects of LV are expected to be very small, and special systems are often used to search it. High-energy astrophysical neutrinos offer a unique system to search signatures of LV, due to the three factors: high neutrino energy, long propagation distance, and the presence of quantum mechanical interference. In this brief review, we introduce tests of LV and summarize existing searches of LV, using atmospheric and astrophysical neutrinos.

scholarly journals Multi-detector approach to enhance the sensitivity of neutrino telescopes to low-energy astrophysical sources

2021 ◽  
Vol 16 (12) ◽  
pp. C12012
Author(s):  
G. de Wasseige
Keyword(s):  
Energy Range ◽  
Neutrino Flux ◽  
High Energy ◽  
Low Energy ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Energy Neutrino ◽  
Astrophysical Neutrinos ◽  
Transient Sources ◽  
The Moment

Abstract While large neutrino telescopes have so far mainly focused on the detection of TeV-PeV astrophysical neutrinos, several efforts are ongoing to extend the sensitivity down to the GeV level for transient sources. Only a handful of neutrino searches have been carried out at the moment leaving the signature of astrophysical transients poorly known in this energy range. In this contribution, we discuss the motivations for high-energy neutrino telescopes to explore the GeV energy range and summarize the current limitations of detectors, such as IceCube and KM3NeT. We then present and compare different approaches for multi-detector analyses that may enhance the sensitivity to a transient GeV neutrino flux.

scholarly journals Constraints on heavy decaying dark matter with current gamma-ray measurements

2021 ◽  
Vol 2021 (11) ◽  
pp. 035
Author(s):  
Marco Chianese ◽  
Damiano F.G. Fiorillo ◽  
Rasmi Hajjar ◽  
Gennaro Miele ◽  
Ninetta Saviano
Keyword(s):  
Dark Matter ◽  
Gamma Rays ◽  
Gamma Ray ◽  
High Energy ◽  
Upper Bounds ◽  
Pierre Auger Observatory ◽  
Telescope Array ◽  
Decay Channels ◽  
Neutrino Telescopes ◽  
Decaying Dark Matter

Abstract Among the several strategies for indirect searches of dark matter, a very promising one is to look for the gamma-rays from decaying dark matter. Here we use the most up-to-date upper bounds on the gamma-ray flux from 105 to 1011 GeV, obtained from CASA-MIA, KASCADE, KASCADE-Grande, Pierre Auger Observatory, Telescope Array and EAS-MSU. We obtain global limits on dark matter lifetime in the range of masses m DM = [107-1015] GeV. We provide the bounds for a set of decay channels chosen as representatives. The constraints derived here are new and cover a region of the parameter space not yet explored. We compare our results with the projected constraints from future neutrino telescopes, in order to quantify the improvement that will be obtained by the complementary high-energy neutrino searches.

scholarly journals A multi-component model for observed astrophysical neutrinos

2018 ◽  
Vol 615 ◽  
pp. A168 ◽  
Author(s):  
Andrea Palladino ◽  
Walter Winter
Keyword(s):  
Gamma Ray ◽  
Probability Distributions ◽  
Neutrino Flux ◽  
Cosmic Ray ◽  
High Energy ◽  
Neutrino Energy ◽  
Point Sources ◽  
Component Model ◽  
Muon Energy ◽  
Astrophysical Neutrinos

Aims. We investigated the origin of observed astrophysical neutrinos. Methods. We propose a multi-component model for the observed diffuse neutrino flux. The model includes residual atmospheric backgrounds, a Galactic contribution (e.g., from cosmic ray interactions with gas), an extragalactic contribution from pp interactions (e.g., from starburst galaxies), and a hard extragalactic contribution from photo-hadronic interactions at the highest energies (e.g., from tidal disruption events or active galactic nuclei). Results. We demonstrate that this model can address the key problems of astrophysical neutrino data, such as the different observed spectral indices in the high-energy starting and through-going muon samples, a possible anisotropy due to Galactic events, the non-observation of point sources, and the constraint from the extragalactic diffuse gamma-ray background. Furthermore, the recently observed muon track with a reconstructed muon energy of 4.5 PeV might be interpreted as evidence for the extragalactic photo-hadronic contribution. We perform the analysis based on the observed events instead of the unfolded fluxes by computing the probability distributions for the event type and reconstructed neutrino energy. As a consequence, we give the probability of each of these astrophysical components on an event-to-event basis.

scholarly journals Sensitivity of multi-PMT optical modules in Antarctic ice to supernova neutrinos of MeV energy

2021 ◽  
Vol 81 (12) ◽  
Author(s):  
C. J. Lozano Mariscal ◽  
L. Classen ◽  
M. A. Unland Elorrieta ◽  
A. Kappes
Keyword(s):  
Optical Sensors ◽  
Detection Rate ◽  
High Energy ◽  
Core Collapse ◽  
South Pole ◽  
False Detection Rate ◽  
The South ◽  
False Detection ◽  
Neutrino Telescopes ◽  
Astrophysical Neutrinos

AbstractNew optical sensors with a segmented photosensitive area are being developed for the next generation of neutrino telescopes at the South Pole. In addition to increasing sensitivity to high-energy astrophysical neutrinos, we show that this will also lead to a significant improvement in sensitivity to MeV neutrinos, such as those produced in core-collapse supernovae (CCSN). These low-energy neutrinos can provide a detailed picture of the events after stellar core collapse, testing our understanding of these violent explosions. We present studies on the event-based detection of MeV neutrinos with a segmented sensor and, for the first time, the potential of a corresponding detector in the deep ice at the South Pole for the detection of extra-galactic CCSN. We find that exploiting temporal coincidences between signals in different photocathode segments, a $$27\ \mathrm {M}_{\odot }$$ 27 M ⊙ progenitor mass CCSN can be detected up to a distance of 341 kpc with a false detection rate of $${0.01}\,\hbox {year}^{-1}$$ 0.01 year - 1 with a detector consisting of 10,000 sensors. Increasing the number of sensors to 20,000 and reducing the optical background by a factor of 70 expands the range such that a CCSN detection rate of 0.1 per year is achieved, while keeping the false detection rate at $${0.01}\,{\hbox {year}^{-1}}$$ 0.01 year - 1 .

scholarly journals Status and first results from the ARCA and ORCA lines of the KM3NeT experiment

2019 ◽  
Vol 209 ◽  
pp. 01006
Author(s):  
Paolo Fermani ◽  
Irene Di Palma
Keyword(s):  
High Energy ◽  
Mass Hierarchy ◽  
Atmospheric Neutrinos ◽  
Neutrino Mass Hierarchy ◽  
Neutrino Telescopes ◽  
Glass Spheres ◽  
Astrophysical Neutrinos ◽  
First Results ◽  
Under Construction ◽  
The Universe

KM3NeT is a network of submarine Cherenkov neutrino telescopes under construction in two different sites in the Mediterranean Sea [1]. The detector at the Italian site, close to the Sicilian coast and named ARCA, will be devoted to the detection of high-energy astrophysical neutrinos coming from sources in the Universe, while the detector at the French site, in the Toulon bay and named ORCA, will exploit atmospheric neutrinos to determine the neutrino mass hierarchy. The telescopes are an array of flexible strings anchored to the sea floor and held close to vertical by submerged buoys. The strings are instrumented with digital optical modules hosted within pressure-resistant glass spheres, each housing 31 3” photomultipliers tubes and the readout electronics. The geometry of the detectors has been adapted to their physics goals. The first calibrations and results of ARCA and ORCA are presented.

scholarly journals Measurement of high energy dark matter from the Sun at IceCube

2021 ◽  
Vol 2021 (12) ◽  
Author(s):  
Ye Xu
Keyword(s):  
Dark Matter ◽  
Energy Range ◽  
High Energy ◽  
The Sun ◽  
Neutrino Telescopes ◽  
Model Based ◽  
Upper Limits ◽  
Matter Model ◽  
Icecube Detector ◽  
Dark Matter Model

Abstract It is assumed that heavy dark matter particles (HDMs) with a mass of O(TeV) are captured by the Sun. HDMs can decay to relativistic light dark matter particles (LDMs), which could be measured by km3 neutrino telescopes (like the IceCube detector). The numbers and fluxes of expected LDMs and neutrinos were evaluated at IceCube with the Z′ portal dark matter model. Based on the assumption that no events are observed at IceCube in 6 years, the corresponding upper limits on LDM fluxes were calculated at 90% C. L.. These results indicated that LDMs could be directly detected in the O(1TeV)-O(10TeV) energy range at IceCube with 100 GeV ≲ mZ′ ≲ 350 GeV and τϕ ≲ 5 × 1022ṡ.

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