Proton and Helium Spectra from the CREAM-III Flight
Primary cosmic-ray elemental spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass (CREAM) experiment since 2004. The third CREAM payload (CREAM-III) flew for 29 days during the 2007-2008 Antarctic season. Energies of incident particles above 1 TeV are measured with a calo...
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ftdatacite:10.48550/arxiv.1704.02512 2023-05-15T13:46:15+02:00 Proton and Helium Spectra from the CREAM-III Flight Yoon, Y. S. Anderson, T. Barrau, A. Conklin, N. B. Coutu, S. Derome, L. Han, J. H. Jeon, J. A. Kim, K. C. Kim, M. H. Lee, H. Y. Lee, J. Lee, M. H. Lee, S. E. Link, J. T. Menchaca-Rocha, A. Mitchell, J. W. Mognet, S. I. Nutter, S. Park, I. H. Picot-Clemente, N. Putze, A. Seo, E. S. Smith, J. Wu, J. 2017 https://dx.doi.org/10.48550/arxiv.1704.02512 https://arxiv.org/abs/1704.02512 unknown arXiv https://dx.doi.org/10.3847/1538-4357/aa68e4 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ High Energy Astrophysical Phenomena astro-ph.HE FOS Physical sciences article-journal Article ScholarlyArticle Text 2017 ftdatacite https://doi.org/10.48550/arxiv.1704.02512 https://doi.org/10.3847/1538-4357/aa68e4 2022-04-01T10:40:26Z Primary cosmic-ray elemental spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass (CREAM) experiment since 2004. The third CREAM payload (CREAM-III) flew for 29 days during the 2007-2008 Antarctic season. Energies of incident particles above 1 TeV are measured with a calorimeter. Individual elements are clearly separated with a charge resolution of ~0.12 e (in charge units) and ~0.14 e for protons and helium nuclei, respectively, using two layers of silicon charge detectors. The measured proton and helium energy spectra at the top of the atmosphere are harder than other existing measurements at a few tens of GeV. The relative abundance of protons to helium nuclei is 9.53+-0.03 for the range of 1 TeV/n to 63 TeV/n. The ratio is considerably smaller than other measurements at a few tens of GeV/n. The spectra become softer above ~20 TeV. However, our statistical uncertainties are large at these energies and more data are needed. Text Antarc* Antarctic DataCite Metadata Store (German National Library of Science and Technology) Antarctic |
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High Energy Astrophysical Phenomena astro-ph.HE FOS Physical sciences |
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High Energy Astrophysical Phenomena astro-ph.HE FOS Physical sciences Yoon, Y. S. Anderson, T. Barrau, A. Conklin, N. B. Coutu, S. Derome, L. Han, J. H. Jeon, J. A. Kim, K. C. Kim, M. H. Lee, H. Y. Lee, J. Lee, M. H. Lee, S. E. Link, J. T. Menchaca-Rocha, A. Mitchell, J. W. Mognet, S. I. Nutter, S. Park, I. H. Picot-Clemente, N. Putze, A. Seo, E. S. Smith, J. Wu, J. Proton and Helium Spectra from the CREAM-III Flight |
topic_facet |
High Energy Astrophysical Phenomena astro-ph.HE FOS Physical sciences |
description |
Primary cosmic-ray elemental spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass (CREAM) experiment since 2004. The third CREAM payload (CREAM-III) flew for 29 days during the 2007-2008 Antarctic season. Energies of incident particles above 1 TeV are measured with a calorimeter. Individual elements are clearly separated with a charge resolution of ~0.12 e (in charge units) and ~0.14 e for protons and helium nuclei, respectively, using two layers of silicon charge detectors. The measured proton and helium energy spectra at the top of the atmosphere are harder than other existing measurements at a few tens of GeV. The relative abundance of protons to helium nuclei is 9.53+-0.03 for the range of 1 TeV/n to 63 TeV/n. The ratio is considerably smaller than other measurements at a few tens of GeV/n. The spectra become softer above ~20 TeV. However, our statistical uncertainties are large at these energies and more data are needed. |
format |
Text |
author |
Yoon, Y. S. Anderson, T. Barrau, A. Conklin, N. B. Coutu, S. Derome, L. Han, J. H. Jeon, J. A. Kim, K. C. Kim, M. H. Lee, H. Y. Lee, J. Lee, M. H. Lee, S. E. Link, J. T. Menchaca-Rocha, A. Mitchell, J. W. Mognet, S. I. Nutter, S. Park, I. H. Picot-Clemente, N. Putze, A. Seo, E. S. Smith, J. Wu, J. |
author_facet |
Yoon, Y. S. Anderson, T. Barrau, A. Conklin, N. B. Coutu, S. Derome, L. Han, J. H. Jeon, J. A. Kim, K. C. Kim, M. H. Lee, H. Y. Lee, J. Lee, M. H. Lee, S. E. Link, J. T. Menchaca-Rocha, A. Mitchell, J. W. Mognet, S. I. Nutter, S. Park, I. H. Picot-Clemente, N. Putze, A. Seo, E. S. Smith, J. Wu, J. |
author_sort |
Yoon, Y. S. |
title |
Proton and Helium Spectra from the CREAM-III Flight |
title_short |
Proton and Helium Spectra from the CREAM-III Flight |
title_full |
Proton and Helium Spectra from the CREAM-III Flight |
title_fullStr |
Proton and Helium Spectra from the CREAM-III Flight |
title_full_unstemmed |
Proton and Helium Spectra from the CREAM-III Flight |
title_sort |
proton and helium spectra from the cream-iii flight |
publisher |
arXiv |
publishDate |
2017 |
url |
https://dx.doi.org/10.48550/arxiv.1704.02512 https://arxiv.org/abs/1704.02512 |
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Antarctic |
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Antarctic |
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Antarc* Antarctic |
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Antarc* Antarctic |
op_relation |
https://dx.doi.org/10.3847/1538-4357/aa68e4 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1704.02512 https://doi.org/10.3847/1538-4357/aa68e4 |
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1766239143977811968 |