Study of Ultra-High Energy Cosmic Ray composition using Telescope Array’s Middle Drum detector and surface array in hybrid mode

Abbasi, Rasha; Abe, M.; Abu‐Zayyad, T.; Allen, M.; Anderson, R. J.; Azuma, R.; Barcikowski, E.; Belz, J. W.; Bergman, D. R.; Blake, S. A.; Cady, R.; Chae, M. J.; Cheon, B. G.; Chiba, J.; Chikawa, M.; Cho, W. R.; Fujii, Toshihiro; Fukushima, M.; Goto, Toru; Hanlon, W.; Hayashi, Y.; Hayashida, N.; Hibino, K.; Honda, K.; Ikeda, D.; Inoue, N.; Ishii, Takaaki; Ishimori, R.; Ito, Hirotaka; Ivanov, D.; Jui, C.; Kadota, K.; Kakimoto, F.; Kalashev, O.; Kasahara, K.; Kawai, H.; Kawakami, S.; Kawana, S.; Kawata, K.; Kido, E.; Kim, H. B.; Kim, J. H.; Kitamura, S.; Kitamura, Yoshihisa; Kuzmin, V.; Kwon, Y. J.; Lan, J.; Lim, S. I.; Lundquist, Jon Paul; Machida, K.; Martens, K.; Matsuda, Toshio; Matsuyama, T.; Matthews, J. N.; Minamino, M.; Mukai, Yoshihiro; Myers, I.; Nagasawa, K.; Nagataki, Shigehiro; Nakamura, Tôru; Nonaka, T.; Nozato, A.; Ogio, S.; Ogura, J.; Ohnishi, M.; Ohoka, H.; Oki, K.; Okuda, Takeshi; Ono, M.; Oshima, A.; Ozawa, S.; Park, I. H.; Пширков, М. С.; Rodriguez, D.; Рубцов, Г.; Ryu, Dongsu; Sagawa, H.; Sakurai, N.; Sampson, Anthony; Scott, L. M.; Shah, P. D.; Shibata, F.; Shibata, T.; Shimodaira, Hidetoshi; Shin, B. K.; Shin, Han-Back; Smith, J. D.; Sokolsky, P.; Springer, R. W.; Stokes, B. T.; Stratton, S. R.; Stroman, T. A.; Suzawa, T.; Takamura, M.; Takeda, M.; Takeishi, R.; Taketa, A.; Takita, M.; Tameda, Y.; Tanaka, Hidekazu; Tanaka, K.; Tanaka, M.; Thomas, S. B.; Thomson, G. B.; Tinyakov, P.; Tkachev, I.; Tokuno, H.; Tomida, T.; Troitsky, S.; Tsunesada, Y.; Tsutsumi, K.; Uchihori, Y.; Udo, S.; Urban, Federico R.; Vasiloff, G.; Wong, Tony; Yamane, R.; Yamaoka, H.; Yamazaki, K.; Yang, J.; Yashiro, K.; Yoneda, Y.; Yoshida, Shigeru; Yoshii, H.; Zollinger, R.; Zundel, Z.

doi:10.1016/j.astropartphys.2014.11.004

Cited by 188 publications

(126 citation statements)

References 19 publications

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“…Good agreement was found between data and a light, nearly protonic, composition, confirming the earlier HiRes stereo measurements. The elongation rate and mean values of X max found by TA were in good agreement with Auger data, but the TA data is incompatible with a pure iron composition over the whole available range of energies (Abbasi et al 2015a). The latest results from both collaborations are presented in Fig.…”

Section: Scientific Backgroundsupporting

confidence: 69%

“Lomonosov” Satellite—Space Observatory to Study Extreme Phenomena in Space

et al. 2017

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V. A. Sadovnichii et al. zations to study some of extreme phenomena in space related to astrophysics, astroparticle physics, space physics, and space biology. The primary goals of this experiment are to study: -Ultra-high energy cosmic rays (UHECR) in the energy range of the Greizen-ZatsepinKuzmin (GZK) cutoff; -Ultraviolet (UV) transient luminous events in the upper atmosphere; -Multi-wavelength study of gamma-ray bursts in visible, UV, gamma, and X-rays; -Energetic trapped and precipitated radiation (electrons and protons) at low-Earth orbit (LEO) in connection with global geomagnetic disturbances; -Multicomponent radiation doses along the orbit of spacecraft under different geomagnetic conditions and testing of space segments of optical observations of space-debris and other space objects; -Instrumental vestibular-sensor conflict of zero-gravity phenomena during space flight. This paper is directed towards the general description of both scientific goals of the project and scientific equipment on board the satellite. The following papers of this issue are devoted to detailed descriptions of scientific instruments.

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Section: Scientific Backgroundsupporting

confidence: 69%

“Lomonosov” Satellite—Space Observatory to Study Extreme Phenomena in Space

et al. 2017

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“…We note that the composition of UHECRs is still debated. Telescope Array group shows that protons are accelerated to UEHCRs energies [20]. However, the Pierre Auger Observatory group reported the X max distributions show that the heavy nucleus become dominant for composition of UHECRs as the energy increases [21].…”

Section: Summary and Future Planmentioning

confidence: 99%

Constraints on acceleration of ultra high-energy cosmic rays in Fermi gamma-ray sources

Kagaya¹,

Yoshida²

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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We investigate the candidates of accelerator of ultra-high-energy cosmic rays (UHECRs) using the multi-wavelength spectral energy distributions, and discuss about the ability to accelerate UHECRs and constrain their physical conditions (acceleration site and size). The current experimental statistics of UHECRs is not sufficient for identification of the sources, although a spatial correlation between the arrival directions of UHECRs and nearby active galactic nuclei (AGNs) has been discussed using the data of the Pierre Auger Observatory and the Telescope Array. Some authors have discussed about the acceleration of UHECRs using various methods. Among them, Pe'er & Loeb (2012) derived constraints on the ability of AGNs to produce UHECRs by using observational quantities which are synchrotron peak luminosity and the peak flux ratio of inverse Compton scattering to synchrotron emission. For adopting this method, we need data of gammaray observation to determine the peak flux for high-energy region due to inverse Compton scattering. Thus, we focused on the Fermi Large Area Telescope gamma-ray sources. We investigated a spatial correlation between AGNs and the arrival directions of UHECRs, and we selected six AGNs as candidates of accelerator of UHECRs. We analyzed their spectral energy distributions by using multi-wavelength archival observational data. By introducing the constraints of Pe'er & Loeb (2012), we evaluate the physical conditions in the acceleration regions of these six AGNs and discuss whether they can accelerate to UHECRs. From the analysis, we found that three AGNs have ability to accelerate UHE protons to UHECRs in the AGN cores. Furthermore, we constrained the minimum size of the acceleration region for each source when UHE particles are accelerated in the AGN lobes. If UHE protons are accelerated, a few kpc-100 kpc are required as the minimum acceleration size. In the case of acceleration of heavy nucleus, the heavy particles can be accelerated in the AGN lobes if the size is larger than a few kpc. In this paper, we show that we achieved to establish a test method for individual candidate sources of acceleration of UHECRs.

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“…• , can measure the depth of shower maximum, X max , to an accuracy of about 20 g/cm 2 [1]. This is sufficient to determine, on a statistical basis, the composition of primary cosmic rays.…”

Section: Introductionmentioning

confidence: 99%

“…This is sufficient to determine, on a statistical basis, the composition of primary cosmic rays. Although in some energy ranges there is disagreement among experiments [1,2,3], from about 10…”

Section: Introductionmentioning

confidence: 99%

Search for EeV Protons of Galactic Origin

Ivanov¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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Cosmic rays in the energy range 10 18.0 -10 18.5 eV are thought to have a light, probably protonic, composition. To study their origin one can search for anisotropy in their arrival directions. Extragalactic cosmic rays should be isotropic, but galactic cosmic rays of this type should be seen mostly along the galactic plane, and there should be a shortage of events coming from directions near the galactic anticenter. This is due to the fact that, under the influence of the galactic magnetic field, the transition from ballistic to diffusive behavior is well advanced, and this qualitative picture persists over the whole energy range. Guided by models of the galactic magnetic field that indicate that the enhancement along the galactic plane should have a standard deviation of about 20• in galactic latitude, and the deficit in the galactic anticenter 2 direction should have a standard deviation of about 50• in galactic longitude, we use the data of the Telescope Array surface detector in 10 18.0 to 10 18.5 eV energy range to search for these effects. The data are isotropic. Neither an enhancement along the galactic plane nor a deficit in the galactic anticenter direction is found. Using these data we place an upper limit on the fraction of EeV cosmic rays of galactic origin at 1.3% at 95% confidence level.

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Study of Ultra-High Energy Cosmic Ray composition using Telescope Array’s Middle Drum detector and surface array in hybrid mode

Cited by 188 publications

References 19 publications

“Lomonosov” Satellite—Space Observatory to Study Extreme Phenomena in Space

“Lomonosov” Satellite—Space Observatory to Study Extreme Phenomena in Space

Constraints on acceleration of ultra high-energy cosmic rays in Fermi gamma-ray sources

Search for EeV Protons of Galactic Origin

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