Journal
ASTRONOMY & ASTROPHYSICS
Volume 508, Issue 2, Pages 561-564Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/200913323
Keywords
cosmic rays; methods: data analysis
Categories
Funding
- CAPES Foundation
- Ministry of Education of Brazil
- German Ministry for Education and Research (BMBF)
- Max Planck Society
- French Ministry for Research
- CNRS-IN2P3
- U. K. Science and Technology Facilities Council (STFC)
- IPNP of the Charles University
- Polish Ministry of Science and Higher Education
- South African Department of Science and Technology
- National Research Foundation
- University of Namibia
- STFC [PP/E001319/1, ST/G003084/1, ST/F002963/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/E001319/1, ST/G003084/1, ST/F002963/1] Funding Source: researchfish
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The measurement of an excess in the cosmic-ray electron spectrum between 300 and 800 GeV by the ATIC experiment has - together with the PAMELA detection of a rise in the positron fraction up to approximate to 100 GeV - motivated many interpretations in terms of dark matter scenarios; alternative explanations assume a nearby electron source like a pulsar or supernova remnant. Here we present a measurement of the cosmic-ray electron spectrum with H. E. S. S. starting at 340 GeV. While the overall electron flux measured by H. E. S. S. is consistent with the ATIC data within statistical and systematic errors, the H. E. S. S. data exclude a pronounced peak in the electron spectrum as suggested for interpretation by ATIC. The H. E. S. S. data follow a power-law spectrum with spectral index of 3.0 +/- 0.1(stat.) +/- 0.3(syst.), which steepens at about 1 TeV.
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