A systematic uncertainty on the energy scale of the Telescope Array fluorescence detectors

Fujii, Toshihiro; Fukushima, M.; Ikeda, D.; Ivanov, D.; Lundquist, Jon Paul; Shin, B. K.; Thomson, Gordon; Tsunesada, Y.

doi:10.22323/1.301.0524

Cited by 5 publications

(3 citation statements)

References 12 publications

(23 reference statements)

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“…A missing energy correction is applied to the reconstructed data and MC showers based on the same composition assumption, with the correction for each primary type and energy being estimated from the CONEX generated showers (cross checked against CORSIKA predictions). We use QGSJet II-3 because, at higher energies, we have measured [40] the missing energy using a technique invented by the Auger collaboration, and found that it agrees well with that predicted by QGSJet II-3. In addition to calculating the aperture, the simulation is also used to verify the accuracy of the event reconstruction procedure.…”

Section: Simulationmentioning

confidence: 65%

The Cosmic-Ray Energy Spectrum between 2 PeV and 2 EeV Observed with the TALE detector in monocular mode

Abbasi,

Abe,

Abu-Zayyad

et al. 2018

Preprint

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We report on a measurement of the cosmic ray energy spectrum by the Telescope Array Low-Energy Extension (TALE) air fluorescence detector. The TALE air fluorescence detector is also sensitive to the Cherenkov light produced by shower particles. Low energy cosmic rays, in the PeV energy range, are detectable by TALE as "Cherenkov Events". Using these events, we measure the energy spectrum from a low energy of ∼ 2 PeV to an energy greater than 100 PeV. Above 100 PeV TALE can detect cosmic rays using air fluorescence. This allows for the extension of the measurement to energies greater than a few EeV. In this paper, we will describe the detector, explain the technique, and present results from a measurement of the spectrum using ∼ 1000 hours of observation. The observed spectrum shows a clear steepening near 10 17.1 eV, along with an ankle-like structure at 10 16.2 eV. These features present important constraints on galactic cosmic rays origin and propagation models. The feature at 10 17.1 eV may also mark the end of the galactic cosmic rays flux and the start of the transition to extra-galactic sources.

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Section: Simulationmentioning

confidence: 65%

The Cosmic-Ray Energy Spectrum between 2 PeV and 2 EeV Observed with the TALE detector in monocular mode

Abbasi,

Abe,

Abu-Zayyad

et al. 2018

Preprint

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“…The estimate for inclined events is extrapolated to low energies. Right:Auger data-driven estimation of E inv compared with the parameterisations for protons, iron and mixed composition reported in [1] and the one in use by Telescope Array [22].…”

Section: Parameterisation Of E Inv As a Function Of E Calmentioning

confidence: 99%

Determination of the invisible energy of extensive air showers from the data collected at Pierre Auger Observatory

Mariazzi

2019

EPJ Web Conf.

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In order to get the primary energy of cosmic rays from their extensive air showers using the fluorescence detection technique, the invisible energy should be added to the measured calorimetric energy. The invisible energy is the energy carried away by particles that do not deposit all their energy in the atmosphere. It has traditionally been calculated using Monte Carlo simulations that are dependent on the assumed primary particle mass and on model predictions for neutrino and muon production. In this work the invisible energy is obtained directly from events detected by the Pierre Auger Observatory. The method applied is based on the correlation of the measurements of the muon number at the ground with the invisible energy of the showers. By using it, the systematic uncertainties related to the unknown mass composition and to the high energy hadronic interaction models are significantly reduced, improving in this way the estimation of the energy scale of the Observatory.

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“…Two FAST telescopes have already been installed at the TA site, in October 2016 and September 2017 [36]. Both telescopes are fully remotely-operable.…”

Section: Fluorescence Detector Array Of Single-pixel Telescopesmentioning

confidence: 99%

Future ground arrays for ultrahigh-energy cosmic rays: recent updates and perspectives

Fujii

2019

EPJ Web Conf.

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The origin and nature of ultrahigh-energy cosmic rays (UHECRs) are one of the most intriguing mysteries in particle astrophysics and astronomy. The two largest observatories, the Pierre Auger Observatory and the Telescope Array Experiment, are steadily observing UHECRs in both hemispheres in order to better understand their origin and associated acceleration mechanisms at the highest energies. We highlight their latest results including on-going upgrades, AugerPrime and TA×4, and then address the requirements for a next-generation observatory. We share recent updates and perspectives for a future ground array of fluorescence detectors, addressing the requirements for a large-area, low-cost detector suitable for measuring the properties of the highest energy cosmic rays with an unprecedented aperture. arXiv:1810.06678v1 [astro-ph.HE]

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A systematic uncertainty on the energy scale of the Telescope Array fluorescence detectors

Cited by 5 publications

References 12 publications

The Cosmic-Ray Energy Spectrum between 2 PeV and 2 EeV Observed with the TALE detector in monocular mode

The Cosmic-Ray Energy Spectrum between 2 PeV and 2 EeV Observed with the TALE detector in monocular mode

Determination of the invisible energy of extensive air showers from the data collected at Pierre Auger Observatory

Future ground arrays for ultrahigh-energy cosmic rays: recent updates and perspectives

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