Search for PeVatrons at the Galactic Center using a radio air-shower array at the South Pole

Haungs, A.; Huege, T.; Schröder, Frank G.

doi:10.1140/epjc/s10052-018-5537-2

Cited by 36 publications

(58 citation statements)

References 34 publications

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“…Also, in the 30 −80 MHz band, the frequency spectrum can not be described by a simple exponential function [36,37], so a more complex parameterization would have to be used, which makes the reconstruction more challenging. Together with an improved signal to noise ratio at higher frequencies [43], this makes the use of frequency bands outside the 30 −80 MHz band an attractive option.…”

Section: Implications For Cosmic-ray Detectorsmentioning

confidence: 99%

Reconstructing the cosmic-ray energy from the radio signal measured in one single station

Gläser

Nelles

2019

J. Cosmol. Astropart. Phys.

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Short radio pulses can be measured from showers of both high-energy cosmic rays and neutrinos. While commonly several antenna stations are needed to reconstruct the energy of an air shower, we describe a novel method that relies on the radio signal measured in one antenna station only. Exploiting a broad frequency bandwidth of 80 − 300 MHz, we obtain a statistical energy resolution of better than 15% on a realistic Monte Carlo set. This method is both a step towards energy reconstruction from the radio signal of neutrino induced showers, as well as a promising tool for cosmic-ray radio arrays. Especially for hybrid arrays where the air shower geometry is provided by an independent detector, this method provides a precise handle on the energy of the shower even with a sparse array.

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Section: Implications For Cosmic-ray Detectorsmentioning

confidence: 99%

Reconstructing the cosmic-ray energy from the radio signal measured in one single station

Gläser

Nelles

2019

J. Cosmol. Astropart. Phys.

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“…To complement studies performed in this energy range by optical detectors, radio detectors should feature the same energy and shower maximum resolution (10% and 20 g/cm 2 respectively). This is crucial for the next-generation radio detectors focused on detection of gamma ray photons [7] and neutrino [8] .…”

Section: Introductionmentioning

confidence: 99%

Reconstruction of cosmic ray air showers with Tunka-Rex data using template fitting of radio pulses

Bezyazeekov¹,

Буднев²,

Chernykh³

et al. 2018

Phys. Rev. D

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We present an improved method for the precise reconstruction of cosmic-ray air showers above 10 17 eV with sparse radio arrays. The method is based on the comparison of measured pulses to predictions for radio pulse shapes by CoREAS simulations. We applied our method to the data of Tunka-Rex, a 1 km 2 radio array in Siberia operating in the frequency band of 30-80 MHz. Tunka-Rex is triggered by the air-Cherenkov detector Tunka-133 and by scintillators (Tunka-Grande). The instrument collects air-shower data since 2012. The present paper describes an updated data analysis of Tunka-Rex and details of the new method applied. After quality cuts, when Tunka-Rex reaches its full efficiency, the energy resolution of about 10% given by the new method has reached the limit of systematic uncertainties due to the calibration uncertainty and shower-to-shower fluctuations. At the same time the shower maximum reconstruction has improved compared to the previous method based on the slope of the lateral distribution and reaches a precision of better than 35 g/cm 2 . We also define conditions of the measurements at which the shower maximum resolution of Tunka-Rex reaches a value of 25 g/cm 2 and becomes competitive to optical detectors. To check and validate our reconstruction and efficiency cuts we compare individual events to the reconstruction of Tunka-133. Furthermore, we compare the mean of the shower maximum as a function of primary energy to the measurements of other experiments.PACS numbers: 96.50.sd, 95.55.Jz, 07.50.Qx,

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“…A proposed scintillator array (Huber et al 2017) at the surface will improve the sensitivity to the electromagnetic shower component and counteract the degradation of the photon sensitivity due to snow accumulation. Furthermore, radio antennas at the surface may improve the gamma-hadron separation and increase the sky coverage such that the Galactic center comes into the FOV (Balagopal et al 2018). In the long term, a 7.9km 3 nextgeneration IceCube detector(van Santen et al 2018) is being designed along with a 75km 2 surface scintillator array.…”

Section: Discussionmentioning

confidence: 99%

Search for PeV Gamma-Ray Emission from the Southern Hemisphere with 5 Yr of Data from the IceCube Observatory

Aartsen¹,

Ackermann²,

Adams³

et al. 2020

ApJ

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The measurement of diffuse PeV gamma-ray emission from the Galactic plane would provide information about the energy spectrum and propagation of Galactic cosmic rays, and the detection of a pointlike source of PeV gamma-rays would be strong evidence for a Galactic source capable of accelerating cosmic rays up to at least a few PeV. This paper presents several unbinned maximum-likelihood searches for PeV gamma-rays in the Southern Hemisphere using 5 yr of data from the IceTop air shower surface detector and the in-ice array of the IceCube Observatory. The combination of both detectors takes advantage of the low muon content and deep shower maximum of gamma-ray air showers and provides excellent sensitivity to gamma-rays between ∼0.6 and 100 PeV. Our measurements of pointlike and diffuse Galactic emission of PeV gamma-rays are consistent with the background, so we constrain the angle-integrated diffuse gamma-ray flux from the Galactic plane at 2 PeV to 2.61×10 −19 cm −2 s −1 TeV −1 at 90% confidence, assuming an E −3 spectrum, and we estimate 90% upper limits on pointlike emission at 2 PeV between 10 −21 and 10 −20 cm −2 s −1 TeV −1 for an E −2 spectrum, depending on decl. Furthermore, we exclude unbroken power-law emission up to 2 PeV for several TeV gamma-ray sources observed by the High Energy Spectroscopic System and calculate upper limits on the energy cutoffs of these sources at 90% confidence. We also find no PeV gamma-rays correlated with neutrinos from IceCube's high-energy starting event sample. These are currently the strongest constraints on PeV gamma-ray emission.

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Search for PeVatrons at the Galactic Center using a radio air-shower array at the South Pole

Cited by 36 publications

References 34 publications

Reconstructing the cosmic-ray energy from the radio signal measured in one single station

Reconstructing the cosmic-ray energy from the radio signal measured in one single station

Reconstruction of cosmic ray air showers with Tunka-Rex data using template fitting of radio pulses

Search for PeV Gamma-Ray Emission from the Southern Hemisphere with 5 Yr of Data from the IceCube Observatory

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