Showing papers by "Harufumi Tsuchiya published in 2014"
TL;DR: The SciBar Cosmic Ray Telescope (SciCRT) is a multi-purpose cosmic-ray detector that was installed at the Instituto Nacional de Astrofisica, Optica y Electronica (INAOE) in eastern Mexico as discussed by the authors.
11 citations
11 Dec 2014-Nuclear Instruments & Methods in Physics Research Section A-accelerators Spectrometers Detectors and Associated Equipment
TL;DR: In this article, the impact of the resonance strength and sample thickness on the accuracy of the areal density derived by NRTA was investigated by measurements at the time-of-flight facility GELINA.
Abstract: The impact of systematic effects on the areal density derived from a neutron resonance transmission analysis (NRTA) is investigated by measurements at the time-of-flight facility GELINA. The experiments were carried out at a 25 m station using metallic natural Cu discs with different thicknesses. To derive the areal density from a fitting to the experimental transmission, the resonance shape analysis code REFIT was used. Large bias effects were observed using recommended resonance parameters. Therefore, neutron resonance parameters, in particular resonance energies and neutron widths, were derived from the transmission data obtained with a 0.25 mm thick Cu metallic sample. These parameters were used to study the impact of the resonance strength and sample thickness on the accuracy of the areal density derived by NRTA.
10 citations
TL;DR: The SciBar Cosmic Ray Telescope (SciCRT) as discussed by the authors is a fully active tracker with 14,848 scintillator bars, whose dimension is 300 cm × 2.5 cm × 1.3 cm.
Abstract: We plan to observe solar neutrons at Mt. Sierra Negra (4,600 m above sea level) in Mexico using the SciBar detector. This project is named the SciBar Cosmic Ray Telescope (SciCRT). The main aims of the SciCRT project are to observe solar neutrons to study the mechanism of ion acceleration on the surface of the sun and to monitor the anisotropy of galactic cosmic-ray muons. The SciBar detector, a fully active tracker, is composed of 14,848 scintillator bars, whose dimension is 300 cm × 2.5 cm × 1.3 cm. The structure of the detector enables us to obtain the particle trajectory and its total deposited energy. This information is useful for the energy reconstruction of primary neutrons and particle identification. The total volume of the detector is 3.0 m × 3.0 m × 1.7 m. Since this volume is much larger than the solar neutron telescope (SNT) in Mexico, the detection efficiency of the SciCRT for neutrons is highly enhanced. We performed the calibration of the SciCRT at Instituto Nacional de Astrofisica, Optica y Electronica (INAOE) located at 2,150 m above sea level in Mexico in 2012. We installed the SciCRT at Mt. Sierra Negra in April 2013 and calibrated this detector in May and August 2013. We started continuous observation in March 2014. In this paper, we report the detector performance as a solar neutron telescope and the current status of the SciCRT.
10 citations
TL;DR: In this article, a simulation study of surrounding material impacts on measurement by 3 He counters was performed with GEANT4 and it was found that a 3 He counter had a small sensitivity to high-energy gamma rays because of inelastic interaction with its cathode-tube materials (Al or stainless steel).
4 citations
26 Mar 2014
TL;DR: M. Amenomori1, X.M. Bi2, D. Chen3, T. Chen4, W. Chen2, S. Cui5, Danzengluobu4, L. Jiang2, F. Ding2, C. Hu2, J. Huang2, H. He2, Z. He5, K. Hibino8, N. Hotta9, Haibing Hu4,H.
Abstract: M. Amenomori1, X. J. Bi2, D. Chen3, T. L. Chen4, W. Y. Chen2, S. W. Cui5, Danzengluobu4, L. K. Ding2, C. F. Feng6, Zhaoyang Feng2, Z. Y. Feng7, Q. B. Gou2, Y. Q. Guo2, H. H. He2, Z. T. He5, K. Hibino8, N. Hotta9, Haibing Hu4, H. B. Hu2, J. Huang2, H. Y. Jia7, L. Jiang2, F. Kajino10, K. Kasahara11, Y. Katayose12, C. Kato13, K. Kawata14, M. Kozai13, Labaciren4, G. M. Le2, A. F. Li15,6,2, H. J. Li4, W. J. Li2,7, C. Liu2, J. S. Liu2, M. Y. Liu4, H. Lu2, X. R. Meng4, K. Mizutani11,16, K. Munakata13, H. Nanjo1, M. Nishizawa17, M. Ohnishi14, I. Ohta18, S. Ozawa11, X. L. Qian6,2, X. B. Qu19,2, T. Saito20, T. Y. Saito21, M. Sakata10, T. K. Sako14, J. Shao2,6, M. Shibata12, A. Shiomi22, T. Shirai8, H. Sugimoto23, M. Takita14, Y. H. Tan2, N. Tateyama8, S. Torii11, H. Tsuchiya24, S. Udo8, H. Wang2, H. R. Wu2, L. Xue6, Y. Yamamoto10, Z. Yang2, S. Yasue25, A. F. Yuan4, T. Yuda14, L. M. Zhai2, H. M. Zhang2, J. L. Zhang2, X. Y. Zhang6, Y. Zhang2, Yi Zhang2, Ying Zhang2, Zhaxisangzhu4, X. X. Zhou7 (The Tibet ASγ Collaboration)