Cosmic ray proton spectrum determined with the imaging atmospheric Cherenkov technique

Aharonian, F.; Akhperjanian, A. G.; Barrio, J. A.; Belgarian, A. S.; Bernlöhr, K.; Beteta, J. J. G.; Bojahr, H.; Bradbury, S. M.; Calle, I. de la; Contreras, J. L.; Cortina, J.; Daum, A.; Deckers, T.; Denninghoff, S.; Fonseca, V.; Gonzalez, J.; Heinzelmann, G.; Hemberger, M.; Hermann, G.; Heß, M.; Heusler, Andréas; Hofmann, W.; Hohl, H.; Holl, I.; Horns, D.; Ibarra, A.; Kankanyan, R.; Kestel, M.; Kirstein, O.; Köhler, Christian; Konopelko, A.; Kornmeyer, H.; Kranich, D.; Krawczynski, H.; Lampeitl, H.; Lindner, A.; Lorenz, E.; Magnussen, N.; Meyer, H.; Mirzoyan, R.; Moralejo, A.; Padilla, L.; Panter, M.; Petry, D.; Plaga, R.; Plyasheshnikov, A.; Prahl, J.; Prosch, C.; Pühlhofer, G.; Rauterberg, Matthias; Renault, C.; Rhode, W.; Röhring, A.; Sahakian, V.; Samorski, M.; Schmele, D.; Schröder, Frank G.; Stamm, W.; Völk, H. J.; Wiebel-Sooth, B.; Wiedner, C. A.; Willmer, M.; Wirth, H.

doi:10.1103/physrevd.59.092003

Cited by 33 publications

(22 citation statements)

References 11 publications

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“…Recently, also indirect measurements of elemental groups became possible, as discussed : Cosmic-ray energy spectra for four groups of elements, from top to bottom: protons, helium, CNO group, and iron group. Protons: Results from direct measurements above the atmosphere by AMS [301], ATIC [302], BESS [303], CAPRICE [304], HEAT [305], [306], IMAX [307], JACEE [308], MASS [309], [310], RUNJOB [284], RICH-II [311], [312], [313], SOKOL [293], [314], and fluxes obtained from indirect measurements by KASCADE electrons and muons for two hadronic interaction models [286] and single hadrons [315], EAS-TOP (electrons and muons) [316] and single hadrons [317], GRAPES-3 interpreted with two hadronic interaction models [318], HEGRA [319], Mt. Chacaltaya [320], Mts.…”

Section: Galactic Cosmic Raysmentioning

confidence: 99%

Cosmic rays from the knee to the highest energies

Blümer¹,

Engel²,

Hörandel

2009

Progress in Particle and Nuclear Physics

277

187

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Section: Galactic Cosmic Raysmentioning

confidence: 99%

Cosmic rays from the knee to the highest energies

Blümer¹,

Engel²,

Hörandel

2009

Progress in Particle and Nuclear Physics

277

187

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“…Thus, the expected trigger rate is estimated to be 4.32±0.07 Hz, which is somewhat higher than the real trigger rate of 2-3 Hz. However, this result is not inconsistent with observations since the fraction of protons in the cosmic ray all particle flux is about 40% (Ichimura et al 1993) and the trigger efficiencies for heavier particles are much smaller than that for protons (Aharonian et al 1999). Image parameter distributions of the above simulated data are shown in Figure 14 in comparison with those of the Vela 1997 data.…”

Section: Appendixmentioning

confidence: 51%

Reanalysis of Data Taken by the Cangaroo 3.8 Meter Imaging Atmospheric Cherenkov Telescope: PSR B1706-44, Sn 1006, and Vela

Yoshikoshi

Mori

Edwards

et al. 2009

ApJ

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We have reanalyzed data from observations of PSR B1706-44, SN 1006, and the Vela pulsar region made with the CANGAROO 3.8 m Imaging Atmospheric Cherenkov Telescope between 1993 and 1998 in response to the results reported for these sources by the H.E.S.S. Collaboration. Although detections of TeV gamma-ray emission from these sources were claimed by CANGAROO more than 10 years ago, upper limits to the TeV gamma-ray signals from PSR B1706-44 and SN 1006 derived by H.E.S.S. are about an order of magnitude lower. The H.E.S.S. group detected strong diffuse TeV gamma-ray emission from Vela but with a morphology differing from the CANGAROO result. In our reanalysis, in which gamma-ray selection criteria have been determined exclusively using gamma-ray simulations and off-source data as background samples, no significant TeV gamma-ray signals have been detected from compact regions around PSR B1706-44 or within the northeast rim of SN 1006. The upper limits to the integral gamma-ray fluxes at the 95% confidence level have been estimated for the 1993 data of PSR B1706-44 to be F (>3.2 ± 1.6 TeV) < 8.03 × 10 −13 photons cm −2 s −1 , for the 1996 and 1997 data of SN 1006 to be F (>3.0 ± 1.5 TeV) < 1.20 × 10 −12 photons cm −2 s −1 and F (>1.8 ± 0.9 TeV) < 1.96 × 10 −12 photons cm −2 s −1 , respectively. We discuss reasons why the original analyses gave the source detections. The reanalysis did result in a TeV gamma-ray signal from the Vela pulsar region at the 4.5σ level using 1993, 1994, and 1995 data. The excess was located at the same position, 0.• 13 to the southeast of the Vela pulsar, as that reported in the original analysis. We have investigated the effect of the acceptance distribution in the field of view of the 3.8 m telescope, which rapidly decreases toward the edge of the field of the camera, on the detected gamma-ray morphology. The expected excess distribution for the 3.8 m telescope has been obtained by reweighting the distribution of HESS J0835-455 measured by H.E.S.S. with the acceptance of the 3.8 m telescope. The result is morphologically comparable to the CANGAROO excess distribution, although the profile of the acceptance-reweighted H.E.S.S. distribution is more diffuse than that of CANGAROO. The integral gamma-ray flux from HESS J0835-455 has been estimated for the same region as defined by H.E.S.S. from the 1993-1995 data of CANGAROO to be F (>4.0 ± 1.6 TeV) = (3.28 ± 0.92) × 10 −12 photons cm −2 s −1 , which is statistically consistent with the integral flux obtained by H.E.S.S.

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“…In this study, a H.E.S.S.-Crab-Nebula-like spectrum [3] was used for the γ-ray signal events (for simplicity the cut-off observed by H.E.S.S. was ignored) and a combination of the proton spectrum measurement of BESS at low energies [4] and HEGRA at high energies [5] is used for the background events. For more details, please refer to [1].…”

Section: Trigger Ratesmentioning

confidence: 99%

Trigger and data rates expected for the CTA observatory

Arribas¹,

Schwanke²,

Wischnewski³

et al. 2012

AIP Conference Proceedings

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The Cherenkov Telescope Array (CTA) is an initiative to build a next-generation observatory for very-high energy γ-rays. Its expected large effective area (O(10 7 m 2 )) and energy threshold as low as 25 GeV imply a challenge for triggering and data acquisition systems. The analysis of the official CTA Monte Carlo production-1 simulations leads to array trigger rates of O(10 kHz) and data rates ranging from O(100 MB/s) to O(1000 MB/s), depending on the read-out scenario. Keywords: gamma rays: observations, instrumentation: detectors PACS: 95.45.+i, 95.55.-n, 95.55.Ka, 95.75.-z, 95.85.Pw, 07.05.Hd High Energy Gamma-Ray Astronomy AIP Conf.

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Cosmic ray proton spectrum determined with the imaging atmospheric Cherenkov technique

Cited by 33 publications

References 11 publications

Cosmic rays from the knee to the highest energies

Cosmic rays from the knee to the highest energies

Reanalysis of Data Taken by the Cangaroo 3.8 Meter Imaging Atmospheric Cherenkov Telescope: PSR B1706-44, Sn 1006, and Vela

Trigger and data rates expected for the CTA observatory

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