scholarly journals Direct measurement of upward-going ultrahigh energy dark matter at the Pierre Auger Observatory

2021 ◽  
Author(s):  
Ye Xu
Keyword(s):  
Dark Matter ◽  
Energy Range ◽  
Pierre Auger Observatory ◽  
Ultrahigh Energy ◽  
Extensive Air Shower ◽  
Air Shower ◽  
The Earth ◽  
Pass Through ◽  
Incoming Energy ◽  
Superheavy Dark Matter

Abstract It is assumed that two types of dark matter particles exist: superheavy dark matter particles (SHDM), the mass of which ∼ inflaton mass, and light fermion dark matter (DM) particles, which are the ultrahigh energy (UHE) products of the decay of SHDM. The Earth will be taken as a detector to search for the UHE DM particles directly. These upward-going particles, which pass through the Earth and air and interact with nuclei, can be detected by the fluorescence detectors (FD) of the Pierre Auger Observatory (Auger), via fluorescent photons due to the development of an extensive air shower. The numbers and fluxes of expected UHE DM particles are evaluated in the incoming energy range between 1 EeV and 1 ZeV with the different lifetimes of decay of SHDM and mass of Z′. According to the Auger data from 2008 to 2019, the upper limit for UHE DM fluxes is also estimated at 90% confidence limit with the FD of Auger. Finally, it is reasonable to make a conclusion that UHE DM particles could be directly detected in the energy range between O(1 EeV) and O(10 EeV) with the FD of Auger. This might prove whether SHDM particles exist in the Universe.

scholarly journals Superheavy dark matter and ultrahigh-energy cosmic rays

2006 ◽  
Vol 84 (6-7) ◽  
pp. 537-543
Author(s):  
R Dick ◽  
K M Hopp ◽  
K E Wunderle
Keyword(s):  
Dark Matter ◽  
Cosmic Rays ◽  
Early Universe ◽  
Cosmic Ray ◽  
Pierre Auger Observatory ◽  
Ultrahigh Energy ◽  
Mass Window ◽  
Ultrahigh Energy Cosmic Rays ◽  
Superheavy Dark Matter ◽  
Arrival Directions

The phase of inflationary expansion in the early Universe produces superheavy relics in a mass window between 1012 and 1014 GeV. Decay or annihilation of these superheavy relics an explain the observed ultrahigh-energy cosmic rays beyond the Greisen–Zatsepin–Kuzmin cutoff. We emphasize that the pattern of cosmic-ray arrival directions seen by the Pierre Auger observatory will decide between the different proposals for the origin of ultrahigh-energy cosmic rays.PACS Nos.: 98.70.Sa, 98.70.–f, 95.35.+d, 14.80.–j

scholarly journals Cosmic Ray Energy Spectrum derived from the Data of EAS Cherenkov Light Arrays in the Tunka Valley

2019 ◽  
Vol 210 ◽  
pp. 01003
Author(s):  
V. Prosin ◽  
I. Astapov ◽  
P. Bezyazeekov ◽  
A. Borodin ◽  
M. Brückner ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Cosmic Rays ◽  
Energy Range ◽  
Cosmic Ray ◽  
Cherenkov Light ◽  
Differential Energy Spectrum ◽  
Extensive Air Shower ◽  
Air Shower

The extensive air shower Cherenkov light array Tunka-133 collected data during 7 winter seasons from 2009 to 2017. From 2175 hours of data taking, we derived the differential energy spectrum of cosmic rays in the energy range 6 · 1015 2 · 1018 eV. The TAIGA-HiSCORE array is in the process of continuous expansion and modernization. Here we present the results obtained with 28 stations of the first HiSCORE stage from 35 clear moonless nights in the winter of 2017-2018. The combined spectrum of two arrays covers a range of 2 · 1014 – 2 · 1018 eV.

DIFFUSED ČERENKOV LIGHT MEASUREMENTS FOR THE EUSO PROJECT

2005 ◽  
Vol 20 (29) ◽  
pp. 6906-6908
Author(s):  
P. VALLANIA ◽  
A. CAPPA ◽  
L. FAVA ◽  
P. GALEOTTI ◽  
O. SAAVEDRA ◽  
...  
Keyword(s):  
Light Transmission ◽  
Uv Light ◽  
Fluorescent Light ◽  
Fluorescent Signal ◽  
Extensive Air Shower ◽  
Air Shower ◽  
The Earth ◽  
Shower Energy ◽  
Cerenkov Light ◽  
Transmission And Reflection

The aim of the EUSO (Extreme Universe Space Observatory) experiment is to measure from space the fluorescent light produced by the interaction of Extreme Energy Cosmic Rays (EECRs) with the Earth atmosphere. Besides the fluorescent signal, a huge amount of Čerenkov photons is emitted in a narrow cone hitting the Earth surface, where it is partially diffused. The detection of this diffused signal, in a delayed coincidence with the fluorescent signal, allows the absolute positioning of the EECR track, while the knowledge of the diffusing properties of the surface gives an independent indication of the shower energy. Measuring simultaneously on ground the electromagnetic component, the direct Čerenkov light, and the diffused Čerenkov light over different surfaces, we aim to characterize the emitted signal as a function of the energy and the arrival direction of the Extensive Air Shower (EAS), and to evaluate its possible detection from space. This is implemented by the ULTRA (Uv Light Transmission and Reflection in the Atmosphere) experiment composed by a small EAS array and a UltraViolet (UV) telescope. The experimental setups used in the first runs at sea level and at 1970 m a.s.l. are described and the first preliminary results are presented.

scholarly journals Galactic Anisotropy of Cosmic Ray Intensity Observed by an Air Shower Experiment

2006 ◽  
Vol 23 (3) ◽  
pp. 129-134
Author(s):  
Mahmud Bahmanabadi ◽  
Mehdi Khakian Ghomi ◽  
Farzaneh Sheidaei ◽  
Jalal Samimi
Keyword(s):  
Daily Variation ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Extensive Air Shower ◽  
Air Shower ◽  
The Earth ◽  
The Galaxy ◽  
Unidirectional Anisotropy ◽  
Galactic Cosmic Ray ◽  
Shower Array

AbstractWe have monitored multi-TeV cosmic rays by a small air shower array in Tehran (35°43′ N, 51°20′ E, 1200 m = 890 g cm−2). More than 1.1 × 106 extensive air shower events were recorded. These observations enabled us to analyse sidereal variation of the galactic cosmic ray intensity. The observed sidereal daily variation is compared to the expected variation which includes the Compton–Getting effect due to the motion of the earth in the Galaxy. In addition to the Compton–Getting effect, an anisotropy has been observed which is due to a unidirectional anisotropy of cosmic ray flow along the Galactic arms.

scholarly journals Ultrahigh Energy Neutrinos at the Pierre Auger Observatory

2013 ◽  
Vol 2013 ◽  
pp. 1-18 ◽  
Author(s):  
P. Abreu ◽  
M. Aglietta ◽  
M. Ahlers ◽  
E. J. Ahn ◽  
I. F. M. Albuquerque ◽  
...  
Keyword(s):  
Pierre Auger Observatory ◽  
Detector Array ◽  
Ultrahigh Energy ◽  
Astroparticle Physics ◽  
Air Showers ◽  
Diffuse Flux ◽  
The Earth ◽  
Surface Detector ◽  
A Priority

The observation of ultrahigh energy neutrinos (UHEνs) has become a priority in experimental astroparticle physics. UHEνs can be detected with a variety of techniques. In particular, neutrinos can interact in the atmosphere (downward-goingν) or in the Earth crust (Earth-skimmingν), producing air showers that can be observed with arrays of detectors at the ground. With the surface detector array of the Pierre Auger Observatory we can detect these types of cascades. The distinguishing signature for neutrino events is the presence of very inclined showers produced close to the ground (i.e., after having traversed a large amount of atmosphere). In this work we review the procedure and criteria established to search for UHEνs in the data collected with the ground array of the Pierre Auger Observatory. This includes Earth-skimming as well as downward-going neutrinos. No neutrino candidates have been found, which allows us to place competitive limits to the diffuse flux of UHEνs in the EeV range and above.

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