High-energy electron observations by PPB-BETS flight in Antarctica

By S. Torii, K. Mizutani, T. Tamura, H. Yamagishi, S. Ohta, M. Namiki, H. Murakami, Y. Katayose, Y. Matsuzaka, T. Yamashita and 16 more. 2008

150 citations recorded by the source corpus.

We have observed cosmic-ray electrons from 10 GeV to 800 GeV by a long duration balloon flight using Polar Patrol Balloon (PPB) in Antarctica. The observation was carried out for 13 days at an average altitude of 35 km in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillators inserted between lead plates with 9 radiation lengths. The performance of the detector has been confirmed by the CERN-SPS beam test and also investigated by Monte-Carlo simulations. New telemetry system using a commercial satellite of Iridium, power supply by solar batteries, and automatic level control using CPU have successfully been developed and operated during the flight. From the long duration balloon observations, we derived the energy spectrum of cosmic-ray electrons in the energy range from 100 GeV to 800 GeV. In addition, for the first time we derived the electron arrival directions above 100 GeV, which is consistent with the isotropic distribution.

Subfields: Biomedical Engineering, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b7ca397ffc64fe313a7d7d63030b6b5273953a18

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In Nuclear and High Energy Physics

1. R. Essig
2. P. Schuster
3. N. Toro
4. I. Cholis
5. P. Serpico
6. J. Gelfand
7. Dmitry Malyshev
8. Atlas Collaboration

Citations in the corpus

• Probing dark forces and light hidden sectors at low-energy e+e- colliders (2009, methodology): “The local electron/positron excesses reported by HEAT [1], PAMELA [2, 3], PPB-BETS [ 4 ], ATIC [5], and others [6, 7] are suggestive of weak-scale dark matter interacting with a new light boson, for which the U(1)D is a natural candidate if its mass is O(GeV).”
• Pulsars versus dark matter interpretation of ATIC/PAMELA (2009, background): “[3] S.”
• Astrophysical models for the origin of the positron (2011, methodology): “Figure 2: Electron plus positron fluxes published since 2008 by PPBBETS [5] (statistical errors only), ATIC [6] (statistical e rrors only), HESS [7, 9] (statistical errors only) Fermi [8, 10], as well a s thee spectra recently published by PAMELA [11] and the e ande spectra recently presented by Fer”