Abstract
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 ≈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.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 561-564 |
| Number of pages | 4 |
| Journal | Astronomy and Astrophysics |
| Volume | 508 |
| Issue number | 2 |
| DOIs | |
| State | Published - 2009 |
Keywords
- Cosmic rays
- Methods: data analysis
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Probing the ATIC peak in the cosmic-ray electron spectrum with H.E.S.S. / Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Barres De Almeida, U.; Bazer-Bachi, A. R.; Becherini, Y.; Behera, B.; Bernlöhr, K.; Bochow, A.; Boisson, C.; Bolmont, J.; Borrel, V.; Brucker, J.; Brun, F.; Brun, P.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C G; Cheesebrough, A.; Chounet, L. M.; Clapson, A. C.; Coignet, G.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; Drury, L. O.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Farnier, C.; Feinstein, F.; Fiasson, A.; Förster, A.; Fontaine, G.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gérard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Göring, D.; Hauser, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Holleran, M.; Hoppe, S.; Horns, D.; Jacholkowska, A.; De Jager, O. C.; Jahn, C.; Jung, I.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kendziorra, E.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Keogh, D.; Kluźniak, W.; Kneiske, T.; Komin, Nu; Kosack, K.; Kossakowski, R.; Lamanna, G.; Lenain, J. P.; Lohse, T.; Marandon, V.; Martin, J. M.; Martineau-Huynh, O.; Marcowith, A.; Masbou, J.; Maurin, D.; McComb, T. J L; Medina, M. C.; Moderski, R.; Moulin, E.; Naumann-Godo, M.; De Naurois, M.; Nedbal, D.; Nekrassov, D.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J. F.; De Oña Wilhelmi, E.; Orford, K. J.; Ostrowski, M.; Panter, M.; Paz Arribas, M.; Pedaletti, G.; Pelletier, G.; Petrucci, P. O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raubenheimer, B. C.; Raue, M.; Rayner, S. M.; Reimer, O.; Renaud, M.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schröder, R.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sikora, M.; Skilton, J. L.; Sol, H.; Spangler, D.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Superina, G.; Szostek, A.; Tam, P. H.; Tavernet, J. P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; Van Eldik, C.; Vasileiadis, G.; Venter, C.; Venter, L.; Vialle, J. P.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Wagner, S. J.; Ward, M.; Zdziarski, A. A.; Zech, A.
In: Astronomy and Astrophysics, Vol. 508, No. 2, 2009, p. 561-564.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - Probing the ATIC peak in the cosmic-ray electron spectrum with H.E.S.S.
AU - Aharonian, F.
AU - Akhperjanian, A. G.
AU - Anton, G.
AU - Barres De Almeida, U.
AU - Bazer-Bachi, A. R.
AU - Becherini, Y.
AU - Behera, B.
AU - Bernlöhr, K.
AU - Bochow, A.
AU - Boisson, C.
AU - Bolmont, J.
AU - Borrel, V.
AU - Brucker, J.
AU - Brun, F.
AU - Brun, P.
AU - Bühler, R.
AU - Bulik, T.
AU - Büsching, I.
AU - Boutelier, T.
AU - Chadwick, P. M.
AU - Charbonnier, A.
AU - Chaves, R. C G
AU - Cheesebrough, A.
AU - Chounet, L. M.
AU - Clapson, A. C.
AU - Coignet, G.
AU - Dalton, M.
AU - Daniel, M. K.
AU - Davids, I. D.
AU - Degrange, B.
AU - Deil, C.
AU - Dickinson, H. J.
AU - Djannati-Ataï, A.
AU - Domainko, W.
AU - Drury, L. O.
AU - Dubois, F.
AU - Dubus, G.
AU - Dyks, J.
AU - Dyrda, M.
AU - Egberts, K.
AU - Emmanoulopoulos, D.
AU - Espigat, P.
AU - Farnier, C.
AU - Feinstein, F.
AU - Fiasson, A.
AU - Förster, A.
AU - Fontaine, G.
AU - Füßling, M.
AU - Gabici, S.
AU - Gallant, Y. A.
AU - Gérard, L.
AU - Gerbig, D.
AU - Giebels, B.
AU - Glicenstein, J. F.
AU - Glück, B.
AU - Goret, P.
AU - Göring, D.
AU - Hauser, D.
AU - Hauser, M.
AU - Heinz, S.
AU - Heinzelmann, G.
AU - Henri, G.
AU - Hermann, G.
AU - Hinton, J. A.
AU - Hoffmann, A.
AU - Hofmann, W.
AU - Holleran, M.
AU - Hoppe, S.
AU - Horns, D.
AU - Jacholkowska, A.
AU - De Jager, O. C.
AU - Jahn, C.
AU - Jung, I.
AU - Katarzyński, K.
AU - Katz, U.
AU - Kaufmann, S.
AU - Kendziorra, E.
AU - Kerschhaggl, M.
AU - Khangulyan, D.
AU - Khélifi, B.
AU - Keogh, D.
AU - Kluźniak, W.
AU - Kneiske, T.
AU - Komin, Nu
AU - Kosack, K.
AU - Kossakowski, R.
AU - Lamanna, G.
AU - Lenain, J. P.
AU - Lohse, T.
AU - Marandon, V.
AU - Martin, J. M.
AU - Martineau-Huynh, O.
AU - Marcowith, A.
AU - Masbou, J.
AU - Maurin, D.
AU - McComb, T. J L
AU - Medina, M. C.
AU - Moderski, R.
AU - Moulin, E.
AU - Naumann-Godo, M.
AU - De Naurois, M.
AU - Nedbal, D.
AU - Nekrassov, D.
AU - Nicholas, B.
AU - Niemiec, J.
AU - Nolan, S. J.
AU - Ohm, S.
AU - Olive, J. F.
AU - De Oña Wilhelmi, E.
AU - Orford, K. J.
AU - Ostrowski, M.
AU - Panter, M.
AU - Paz Arribas, M.
AU - Pedaletti, G.
AU - Pelletier, G.
AU - Petrucci, P. O.
AU - Pita, S.
AU - Pühlhofer, G.
AU - Punch, M.
AU - Quirrenbach, A.
AU - Raubenheimer, B. C.
AU - Raue, M.
AU - Rayner, S. M.
AU - Reimer, O.
AU - Renaud, M.
AU - Rieger, F.
AU - Ripken, J.
AU - Rob, L.
AU - Rosier-Lees, S.
AU - Rowell, G.
AU - Rudak, B.
AU - Rulten, C. B.
AU - Ruppel, J.
AU - Sahakian, V.
AU - Santangelo, A.
AU - Schlickeiser, R.
AU - Schöck, F. M.
AU - Schröder, R.
AU - Schwanke, U.
AU - Schwarzburg, S.
AU - Schwemmer, S.
AU - Shalchi, A.
AU - Sikora, M.
AU - Skilton, J. L.
AU - Sol, H.
AU - Spangler, D.
AU - Stawarz, L.
AU - Steenkamp, R.
AU - Stegmann, C.
AU - Stinzing, F.
AU - Superina, G.
AU - Szostek, A.
AU - Tam, P. H.
AU - Tavernet, J. P.
AU - Terrier, R.
AU - Tibolla, O.
AU - Tluczykont, M.
AU - Van Eldik, C.
AU - Vasileiadis, G.
AU - Venter, C.
AU - Venter, L.
AU - Vialle, J. P.
AU - Vincent, P.
AU - Vivier, M.
AU - Völk, H. J.
AU - Volpe, F.
AU - Wagner, S. J.
AU - Ward, M.
AU - Zdziarski, A. A.
AU - Zech, A.
N1 - Copyright: Copyright 2013 Elsevier B.V., All rights reserved.
PY - 2009
Y1 - 2009
N2 - 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 ≈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.
AB - 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 ≈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.
KW - Cosmic rays
KW - Methods: data analysis
UR - http://www.scopus.com/inward/record.url?scp=77649202127&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=77649202127&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/200913323
DO - 10.1051/0004-6361/200913323
M3 - Article
AN - SCOPUS:77649202127
VL - 508
SP - 561
EP - 564
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
IS - 2
ER -