Search for annihilating dark matter in the Sun with 3 years of IceCube data
We present results from an analysis looking for dark matter annihilation in the Sun with the IceCube neutrino telescope. Gravitationally trapped dark matter in the Sun’s core can annihilate into Standard Model particles making the Sun a source of GeV neutrinos. IceCube is able to detect neutrinos wi...
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Springer-Verlag
2018
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| Online Access: | http://hdl.handle.net/1721.1/116527 https://orcid.org/0000-0003-4186-4182 https://orcid.org/0000-0001-8866-3826 https://orcid.org/0000-0002-6393-0438 https://orcid.org/0000-0001-6243-1453 https://orcid.org/0000-0001-7909-5812 |
| _version_ | 1826188780824952832 |
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| author | IceCube Collaboration Arguelles Delgado, Carlos A Axani, Spencer Nicholas Collin, G. H. Conrad, Janet Marie Jones, Benjamin James Poyner Moulai, Marjon H. |
| author2 | Massachusetts Institute of Technology. Laboratory for Nuclear Science |
| author_facet | Massachusetts Institute of Technology. Laboratory for Nuclear Science IceCube Collaboration Arguelles Delgado, Carlos A Axani, Spencer Nicholas Collin, G. H. Conrad, Janet Marie Jones, Benjamin James Poyner Moulai, Marjon H. |
| author_sort | IceCube Collaboration |
| collection | MIT |
| description | We present results from an analysis looking for dark matter annihilation in the Sun with the IceCube neutrino telescope. Gravitationally trapped dark matter in the Sun’s core can annihilate into Standard Model particles making the Sun a source of GeV neutrinos. IceCube is able to detect neutrinos with energies > 100 GeV while its low-energy infill array DeepCore extends this to > 10 GeV. This analysis uses data gathered in the austral winters between May 2011 and May 2014, corresponding to 532 days of livetime when the Sun, being below the horizon, is a source of up-going neutrino events, easiest to discriminate against the dominant background of atmospheric muons. The sensitivity is a factor of two to four better than previous searches due to additional statistics and improved analysis methods involving better background rejection and reconstructions. The resultant upper limits on the spin-dependent dark matter-proton scattering cross section reach down to 1.46 × 10 - 5 pb for a dark matter particle of mass 500 GeV annihilating exclusively into τ + τ - particles. These are currently the most stringent limits on the spin-dependent dark matter-proton scattering cross section for WIMP masses above 50 GeV. |
| first_indexed | 2024-09-23T08:04:36Z |
| format | Article |
| id | mit-1721.1/116527 |
| institution | Massachusetts Institute of Technology |
| last_indexed | 2024-09-23T08:04:36Z |
| publishDate | 2018 |
| publisher | Springer-Verlag |
| record_format | dspace |
| spelling | mit-1721.1/1165272022-09-23T10:45:14Z Search for annihilating dark matter in the Sun with 3 years of IceCube data IceCube Collaboration Arguelles Delgado, Carlos A Axani, Spencer Nicholas Collin, G. H. Conrad, Janet Marie Jones, Benjamin James Poyner Moulai, Marjon H. Massachusetts Institute of Technology. Laboratory for Nuclear Science Arguelles Delgado, Carlos A Axani, Spencer Nicholas Collin, G. H. Conrad, Janet Marie Jones, Benjamin James Poyner Moulai, Marjon H. We present results from an analysis looking for dark matter annihilation in the Sun with the IceCube neutrino telescope. Gravitationally trapped dark matter in the Sun’s core can annihilate into Standard Model particles making the Sun a source of GeV neutrinos. IceCube is able to detect neutrinos with energies > 100 GeV while its low-energy infill array DeepCore extends this to > 10 GeV. This analysis uses data gathered in the austral winters between May 2011 and May 2014, corresponding to 532 days of livetime when the Sun, being below the horizon, is a source of up-going neutrino events, easiest to discriminate against the dominant background of atmospheric muons. The sensitivity is a factor of two to four better than previous searches due to additional statistics and improved analysis methods involving better background rejection and reconstructions. The resultant upper limits on the spin-dependent dark matter-proton scattering cross section reach down to 1.46 × 10 - 5 pb for a dark matter particle of mass 500 GeV annihilating exclusively into τ + τ - particles. These are currently the most stringent limits on the spin-dependent dark matter-proton scattering cross section for WIMP masses above 50 GeV. 2018-06-22T17:22:37Z 2018-06-22T17:22:37Z 2017-03 2016-12 2018-06-20T14:15:05Z Article http://purl.org/eprint/type/JournalArticle 1434-6044 1434-6052 http://hdl.handle.net/1721.1/116527 Aartsen, M. G. et al. “Search for Annihilating Dark Matter in the Sun with 3 Years of IceCube Data.” The European Physical Journal C 77, 3 (March 2017): 146 © 2017 The Author(s) https://orcid.org/0000-0003-4186-4182 https://orcid.org/0000-0001-8866-3826 https://orcid.org/0000-0002-6393-0438 https://orcid.org/0000-0001-6243-1453 https://orcid.org/0000-0001-7909-5812 http://dx.doi.org/10.1140/epjc/s10052-017-4689-9 European Physical Journal C: Particles and Fields Creative Commons Attribution 4.0 International License http://creativecommons.org/licenses/by/4.0/ application/pdf Springer-Verlag Springer |
| spellingShingle | IceCube Collaboration Arguelles Delgado, Carlos A Axani, Spencer Nicholas Collin, G. H. Conrad, Janet Marie Jones, Benjamin James Poyner Moulai, Marjon H. Search for annihilating dark matter in the Sun with 3 years of IceCube data |
| title | Search for annihilating dark matter in the Sun with 3 years of IceCube data |
| title_full | Search for annihilating dark matter in the Sun with 3 years of IceCube data |
| title_fullStr | Search for annihilating dark matter in the Sun with 3 years of IceCube data |
| title_full_unstemmed | Search for annihilating dark matter in the Sun with 3 years of IceCube data |
| title_short | Search for annihilating dark matter in the Sun with 3 years of IceCube data |
| title_sort | search for annihilating dark matter in the sun with 3 years of icecube data |
| url | http://hdl.handle.net/1721.1/116527 https://orcid.org/0000-0003-4186-4182 https://orcid.org/0000-0001-8866-3826 https://orcid.org/0000-0002-6393-0438 https://orcid.org/0000-0001-6243-1453 https://orcid.org/0000-0001-7909-5812 |
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