Naohiro Sone

Shinshu University

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Co-Authors

Y. Tsunesada

Osaka Metropolitan University

M. Kuznetsov

Institute for Nuclear Research

Y. Tameda

Osaka Electro-Communication University

Ryuji Takeishi

The University of Tokyo

M. Ono

RIKEN

Hirokazu Iwakura

Shinshu University

K. Fujita

The University of Tokyo

D. R. Bergman

University of Utah

O. Kalashev

Institute for Nuclear Research

T. Seki

Shinshu University

Cooperative Institutions

Consejo Nacional de Investigaciones Científicas y Técnicas

527

Instituto de Tecnologías en Detección y Astropartículas

445

University of Buenos Aires

419

Universidad Nacional de La Plata

417

National University of General San Martín

389

Pierre Auger Observatory

377

Institute of Astronomy and Space Physics

377

National Technological University

374

Institute of Scientific and Technical Research for Defense

271

Karlsruhe Institute of Technology

191

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Joint analysis of the energy spectrum of ultra-high-energy cosmic rays as measured at the Pierre Auger Observatory and the Telescope Array

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019) (2021)

Y. Tsunesada Rasha Abbasi T. Abu‐Zayyad Monica Allen Yuto Arai

The measurement of the energy spectrum of ultra-high-energy cosmic rays (UHECRs) is of crucial importance to clarify their origin and acceleration mechanisms. The Pierre Auger Observatory in Argentina and the Telescope Array (TA) in the US have reported their measurements of UHECR energy spectra observed in the southern and northern hemisphere, respectively. The region of the sky accessible to both Observatories ($[-15,+24]$ degrees in declination) can be used to cross-calibrate the two spectra. The Auger-TA energy spectrum working group was organized in 2012 and has been working to understand the uncertainties in energy scale in both experiments, their systematic differences, and differences in the shape of the spectra. In previous works, we reported that there was an overall agreement of the energy spectra measured by the two observatories below 10 EeV while at higher energies, a remaining significant difference was observed in the common declination band. We revisit this issue to understand its origin by examining the systematic uncertainties, statistical effects, and other possibilities. We will also discuss the differences in the spectra in different declination bands and a new feature in the spectrum recently reported by the Auger Collaboration.

Pierre Auger Observatory

Right ascension

10.22323/1.395.0337

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The UHECR dipole and quadrupole in the latest data from the original Auger and TA surface detectors

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019) (2021)

P. Tinyakov Rogério de Almeida Rasha Abbasi T. Abu‐Zayyad Monica Allen

The sources of ultra-high-energy cosmic rays are still unknown, but assuming standard physics, they are expected to lie within a few hundred megaparsecs from us. Indeed, over cosmological distances cosmic rays lose energy to interactions with background photons, at a rate depending on their mass number and energy and properties of photonuclear interactions and photon backgrounds. The universe is not homogeneous at such scales, hence the distribution of the arrival directions of cosmic rays is expected to reflect the inhomogeneities in the distribution of galaxies; the shorter the energy loss lengths, the stronger the expected anisotropies. Galactic and intergalactic magnetic fields can blur and distort the picture, but the magnitudes of the largest-scale anisotropies, namely the dipole and quadrupole moments, are the most robust to their effects. Measuring them with no bias regardless of any higher-order multipoles is not possible except with full-sky coverage. In this work, we achieve this in three energy ranges (approximately 8--16 EeV, 16--32 EeV, and 32--$\infty$ EeV) by combining surface-detector data collected at the Pierre Auger Observatory until 2020 and at the Telescope Array (TA) until 2019, before the completion of the upgrades of the arrays with new scintillator detectors. We find that the full-sky coverage achieved by combining Auger and TA data reduces the uncertainties on the north-south components of the dipole and quadrupole in half compared to Auger-only results.

Pierre Auger Observatory

10.22323/1.395.0375

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A study of analysis method for the identification of UHECR source type

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019) (2021)

Fugo Yoshida Rasha Abbasi T. Abu‐Zayyad Monica Allen Yuto Arai

The autocorrelation analysis using the arrival direction of Ultra High Energy Cosmic Rays (UHECRs) has been previously reported by the Telescope Array (TA) experiment. It is expected that the autocorrelation function reflects the source distribution. We simulate the expected arrival direction distribution of the cosmic rays using the catalogs of candidate sources. We take into account random deflection in the magnetic fields, with the magnitude of deflection determined by the charge and energy of the cosmic rays, coherence length and magnitude of the extragalactic magnetic field (EGMF), and by distance to source. In addition, in order to compare with the results of TA experiment, we consider the TA exposure. We compare the autocorrelation of the arrival directions corresponding to different source catalogs with the isotropic distribution. We calculate the autocorrelation function for each type of source candidates using this procedure. We will discuss the ability of this method to identify the source type of UHECRs.

10.22323/1.395.0242

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Measurement of the proton-air cross section with Telescope Array’s Black Rock Mesa and Long Ridge fluorescence detectors, and surface array in hybrid mode

Physical review. D/Physical review. D. (2020)

Rasha Abbasi Mitsuru Abe T. Abu‐Zayyad M. Allen R. Azuma

Ultrahigh energy cosmic rays provide the highest known energy source in the Universe to measure proton cross sections. Though conditions for collecting such data are less controlled than an accelerator environment, current generation cosmic ray observatories have large enough exposures to collect significant statistics for a reliable measurement for energies above what can be attained in the laboratory. Cosmic ray measurements of cross section use atmospheric calorimetry to measure depth of air shower maximum (${X}_{\mathrm{max}}$), which is related to the primary particle's energy and mass. The tail of the ${X}_{\mathrm{max}}$ distribution is assumed to be dominated by showers generated by protons, allowing measurement of the inelastic proton-air cross section. In this work, the proton-air inelastic cross section measurement, ${\ensuremath{\sigma}}_{\mathrm{p}\text{-air}}^{\mathrm{inel}}$, using data observed by Telescope Array's Black Rock Mesa and Long Ridge fluorescence detectors and surface detector array in hybrid mode is presented. ${\ensuremath{\sigma}}_{\mathrm{p}\text{-air}}^{\mathrm{inel}}$ is observed to be $520.1\ifmmode\pm\else\textpm\fi{}35.8{[\mathrm{Stat}]}_{\ensuremath{-}42.9}^{+25.3}[\mathrm{Sys}]\text{ }\text{ }\mathrm{mb}$ at $\sqrt{s}=73\text{ }\text{ }\mathrm{TeV}$. The total proton-proton cross section is subsequently inferred from Glauber formalism and is found to be ${\ensuremath{\sigma}}_{\mathrm{pp}}^{\mathrm{tot}}={139.4}_{\ensuremath{-}21.3}^{+23.4}[\mathrm{Stat}{]}_{\ensuremath{-}25.4}^{+15.7}[\mathrm{Sys}]\text{ }\text{ }\mathrm{mb}$.

Air shower

Glauber

10.1103/physrevd.102.062004

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UHECR mass composition from anisotropy of their arrival directions with the Telescope Array SD

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019) (2021)

M. Kuznetsov P. Tinyakov Rasha Abbasi T. Abu‐Zayyad Monica Allen

We propose a new method for the estimation of ultra-high energy cosmic ray (UHECR) mass composition from a distribution of their arrival directions. The method employs a test statistic (TS) based on a characteristic deflection of UHECR events with respect to the distribution of luminous matter in the local Universe modeled with a flux-weighed 2MRS catalog. Making realistic simulations of the mock UHECR sets, we show that this TS is robust to the presence of galactic and non-extreme extra-galactic magnetic fields and sensitive to the mass composition of events in a set. We apply the method to Telescope Array surface detector data for 11 years and derive new independent constraints on fraction of protons and iron in p-Fe mix at $E > 10$ EeV. At $10 < E < 100$ EeV the data favors increase of allowed proton fraction and decrease of allowed iron fraction, while at $E > 100$ EeV --- pure iron or even more massive composition. This result is in tension with Auger composition model inferred from spectrum-$X_{max}$ fit at $2.7\sigma$ ($2.0\sigma$) for PT'11 (JF'12) regular GMF model.

Mass fraction

10.22323/1.395.0294

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Navigation system of Japanese folding paper based on the 3DCG animation

Naohiro Sone Yoshiaki Shindo

Japanese folding paper is one of Japanese historical culture. Recently, it's used for rehabilitation or applied for structure analysis of industrial packing. However, Japanese folding paper may be recognized as a plaything for children in Japan. Otherwise it is recognized as a good educational material for low aged children in the world. But teaching tool of Japanese folding paper for children in English world has not been developed. To spread the Japanese folding paper to the world by improving the teaching method, we developed the navigation system of Japanese folding paper named PCML (Paper Craft making Language) and PCML browser. PCML shows the Japanese folding paper as the 3DCG animation with collision detection algorithm we developed. In this paper, we describe the detail of PCML and PCML browser.

Folding (DSP implementation)

Craft

10.1109/icalt.2005.209

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Surface detectors of the TAx4 experiment

arXiv (Cornell University) (2021)

Rasha Abbasi Mitsuru Abe T. Abu-Zayyad M. Allen Yuto Arai

Telescope Array (TA) is the largest ultrahigh energy cosmic-ray (UHECR) observatory in the Northern Hemisphere. It explores the origin of UHECRs by measuring their energy spectrum, arrival-direction distribution, and mass composition using a surface detector (SD) array covering approximately 700 km$^2$ and fluorescence detector (FD) stations. TA has found evidence for a cluster of cosmic rays with energies greater than 57 EeV. In order to confirm this evidence with more data, it is necessary to increase the data collection rate.We have begun building an expansion of TA that we call TAx4. In this paper, we explain the motivation, design, technical features, and expected performance of the TAx4 SD. We also present TAx4's current status and examples of the data that have already been collected.

Source

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Effects of Galactic magnetic field on the UHECR anisotropy studies

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019) (2021)

Ryo Higuchi K. Kawata Rasha Abbasi T. Abu‐Zayyad Monica Allen

Telescope Array (TA) and Auger experiments reported anisotropies in the arrival direction of ultra-high-energy cosmic rays (UHECRs). In particular, Auger Collaboration reported a correlation between UHECR events and the flux model of assumed sources and suggested a contribution of starburst galaxies (SBGs) to the anisotropy of UHECRs. However, in their study, the effect of coherent deflections by the galactic magnetic field (GMF) is not taken into account. In this study, we investigated the effect of the GMF on the arrival directions of UHECRs using the cosmic ray propagation code CRPropa3. We used a backtracking technique which consists of propagating antiparticles to map the flux outside the galaxy to at the earth. We estimate the systematic effects caused by GMF in the reported likelihood analysis. We conduct likelihood analysis for mock UHECR datasets based on the flux pattern through the GMF model. We found systematic decrease of $(f_{\rm ani}, \:\theta)$ due to GMF. As prospects for the TAx4 experiment and joint analysis of Auger and TA collaborations, we develop the likelihood analysis method with the convolution of the rigidity spectrum.

Air shower

10.22323/1.395.0358

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Surface detectors of the TAx4 experiment

Nuclear Instruments and Methods in Physics Research Section A Accelerators Spectrometers Detectors and Associated Equipment (2021)

Telescope Array Collaboration Rasha Abbasi Mitsuru Abe T. Abu-Zayyad Monica Allen

Telescope Array (TA) is the largest ultrahigh energy cosmic-ray (UHECR) observatory in the Northern Hemisphere. It explores the origin of UHECRs by measuring their energy spectrum, arrival-direction distribution, and mass composition using a surface detector (SD) array covering approximately 700 km2 and fluorescence detector (FD) stations. TA has found evidence for a cluster of cosmic rays with energies greater than 57 EeV. In order to confirm this evidence with more data, it is necessary to increase the data collection rate. We have begun building an expansion of TA that we call TAx4. In this paper, we explain the motivation, design, technical features, and expected performance of the TAx4 SD. We also present TAx4’s current status and examples of the data that have already been collected.

10.1016/j.nima.2021.165726

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Citations (15)

The status of the TALE surface detector array and TALE infill project

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019) (2021)

S. Ogio Rasha Abbasi T. Abu‐Zayyad Monica Allen Yuto Arai

Routine hybrid observations of the surface detectors (SD) in conjunction with the fluorescence detectors (FD) of the Telescope Array Low-energy Extension (TALE) began in November 2018. In this presentation, we will describe the simulation studies of detector aperture and resolution of the TALE SD, and report on the latest observation results other than the energy spectrum. We are also in the process of expanding the experiment by 50 SDs, with even smaller nearest-neighbor spacing, in order lower the energy threshold to match that of the Cherenkov-dominated events seen by the FD. Details of the upgrade and expected performance of this new extension will be discussed.

Upgrade

Aperture (computer memory)

10.22323/1.395.0255

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Citations (1)