High-energy Electron Spectrum From PPB-BETS Experiment In Antarctica Kenji Yoshida 1, Shoji Torii 2 on behalf of the PPB-BETS collaboration 1 Shibaura.

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High-energy Electron Spectrum From PPB-BETS Experiment In Antarctica Kenji Yoshida 1, Shoji Torii 2 on behalf of the PPB-BETS collaboration 1 Shibaura Institute of Technology, Japan 2 Waseda University, Japan

March 3, 20102HEAD 2010 Side view of the detector 9 r.l. Trajectory of PPB-BETS PPB-BETS Observations in Antarctica Observation: 13 days in Jan days in Jan Altitude: ~35km Altitude: ~35km PPB-BETS : Imaging calorimeter Event selection Event selection Energy measurements Energy measurements Direction measurements Direction measurements

Electron Selection - Proton Rejection - Proton rejection by using the lateral spread of the cascade shower R.E. parameter = Ratio of energy deposition within 5mm from the shower axis to the total March 3, 2010HEAD Observed Events 100GeV Electrons 250GeV Protons R.E. distributions Electron Candidate Proton Candidate

Electron Selection - Gamma-ray Rejection - Fiber signals along the shower axis at top layer => Separation between electrons and gamma rays March 3, 2010HEAD Electron Candidate Gamma-ray Candidate e gamma Distributions of the nearest hit fiber positions from the shower axis

Determination of Electron Energy March 3, 2010HEAD The number of shower particles at shower maximum => Electron energy The number of shower particles at shower maximum => Electron energy

Electron Energy Spectrum - BETS+PPB-BETS - March 3, 2010HEAD A power-law spectrum : Acceptable at the 95% C.L.  2 = (d.o.f.=11)

Search for Anisotropies of Cosmic-ray Electrons above 100GeV March 3, 2010HEAD => No significant anisotropies within statistical errors Ratio of the observed arrival distribution (>100GeV) to isotropic distribution along the Galactic longitude

Summary BETS + PPB-BETS cosmic-ray electron spectrum from 10GeV to 800GeV: => A power-law spectrum E Search for cosmic-ray electron anisotropies above 100GeV by PPB-BETS: => Isotropic distribution within statistical errors For detection of nearby source signatures => Electron observation up to 10 TeV by CALET March 3, 2010HEAD 20108

Backup March 3, 2010HEAD 20109

4 July th ICRC (Merida)10 Effective Geometrical Factor (S  ) Simulation under the same condition of the observations and analysis

4 July th ICRC (Merida)11 Derivation of Cosmic-Ray Electron Energy Spectrum ◆ N e : The Number of electron candidates ◆ C RE : Correction factor of proton contamination in the R.E. cut with energy dependence (~0.68) ◆ C eg : Correction factor of gamma-ray contamination (~0.84) ◆ C enh : Correction of enhancement of flux due to the energy resolution (0.97) ◆ C 2nd : Correction of secondary electrons in the atmosphere (1.3x10 -5 (m -2 s -1 sr -1 GeV -1 ◆ C atm : Correction of energy loss of primary electrons in the overlying atmosphere (1.37)

4 July th ICRC (Merida)12 Uncertainty of Determination of Arrival Directions Angular resolution with scintillating fibers of PPB-BETS detector: ~0.5 deg Differences between Geomagnetic Aspect Sensor and Sun Aspect Sensor: ~5 deg

Atmospheric Gamma-ray Spectrum March 3, 2010HEAD => Consistent with ECC

Proton Rejection Power March 3, 2010HEAD Reduction of proton background: Total Rejection Power of Protons: ~20 x 10 x 20 = 4x 10 3 On-board Trigger by the 1st and 2nd levels: ~ 95 % Selection of Contained Events in Detector: ~ 90 % Lateral spread of cascade shower: ~95 %

4 July th ICRC (Merida)15 Basic Parameters of PPB-BETS Instrument Weight~200 kg Total Weight (including ballast)~480 kg Power Consumption70 W Data Transfer Rate (Iridium Phone)2.4 kbps (Down Link to the Station)64 kbps Energy Range10~1000 GeV Geometrical Factor (SW)500 ~ 600 cm 2 sr Energy Resolution10~25 % Angular Resolution0.35 ~ 0.60 deg.