Hunting for heavy winos in the Galactic Center
Observing gamma rays using ground-based atmospheric Cherenkov telescopes provides one of the only probes of heavy weakly interacting dark matter. A canonical target is the thermal wino, for which the strongest limits come from searches for photon lines from annihilations in the Galactic Center. Irre...
| Main Authors: | , , , , , , , , |
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| Format: | Article |
| Language: | English |
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American Physical Society
2018
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| Online Access: | http://hdl.handle.net/1721.1/119830 https://orcid.org/0000-0003-3472-7606 https://orcid.org/0000-0001-9699-9047 https://orcid.org/0000-0003-0248-0979 |
| _version_ | 1811086243766730752 |
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| author | Rinchiuso, Lucia Moult, Ian Moulin, Emmanuel Baumgart, Matthew Cohen, Timothy Vaidya, Varun Rodd, Nicholas Llewellyn Slatyer, Tracy Robyn Stewart, Iain W |
| author2 | Massachusetts Institute of Technology. Center for Theoretical Physics |
| author_facet | Massachusetts Institute of Technology. Center for Theoretical Physics Rinchiuso, Lucia Moult, Ian Moulin, Emmanuel Baumgart, Matthew Cohen, Timothy Vaidya, Varun Rodd, Nicholas Llewellyn Slatyer, Tracy Robyn Stewart, Iain W |
| author_sort | Rinchiuso, Lucia |
| collection | MIT |
| description | Observing gamma rays using ground-based atmospheric Cherenkov telescopes provides one of the only probes of heavy weakly interacting dark matter. A canonical target is the thermal wino, for which the strongest limits come from searches for photon lines from annihilations in the Galactic Center. Irreducible finite energy resolution effects motivate refining the prediction for a wino signal beyond the photon line approximation; recently, modern effective field theory techniques have been utilized to obtain a precise calculation of the full photon energy spectrum from wino annihilation. In this paper, we investigate the implications for a realistic mock H.E.S.S.-like line search. We emphasize the impact of including the non-trivial spectral shape, and we carefully treat the region of interest, presenting results for choices between 1° and 4° from the Galactic Center. Projected limits for wino masses from 1–70 TeV are interpreted as a constraint on the wino annihilation rate, or alternatively as the minimum core size required such that the wino is not excluded. If there is a thermal wino, H.E.S.S. will be able to probe cores of several kpc, which would begin to cause tension between this dark matter candidate and astrophysical observations/simulations. |
| first_indexed | 2024-09-23T13:23:06Z |
| format | Article |
| id | mit-1721.1/119830 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T13:23:06Z |
| publishDate | 2018 |
| publisher | American Physical Society |
| record_format | dspace |
| spelling | mit-1721.1/1198302022-09-28T13:48:20Z Hunting for heavy winos in the Galactic Center Rinchiuso, Lucia Moult, Ian Moulin, Emmanuel Baumgart, Matthew Cohen, Timothy Vaidya, Varun Rodd, Nicholas Llewellyn Slatyer, Tracy Robyn Stewart, Iain W Massachusetts Institute of Technology. Center for Theoretical Physics Rodd, Nicholas Llewellyn Slatyer, Tracy Robyn Stewart, Iain W Observing gamma rays using ground-based atmospheric Cherenkov telescopes provides one of the only probes of heavy weakly interacting dark matter. A canonical target is the thermal wino, for which the strongest limits come from searches for photon lines from annihilations in the Galactic Center. Irreducible finite energy resolution effects motivate refining the prediction for a wino signal beyond the photon line approximation; recently, modern effective field theory techniques have been utilized to obtain a precise calculation of the full photon energy spectrum from wino annihilation. In this paper, we investigate the implications for a realistic mock H.E.S.S.-like line search. We emphasize the impact of including the non-trivial spectral shape, and we carefully treat the region of interest, presenting results for choices between 1° and 4° from the Galactic Center. Projected limits for wino masses from 1–70 TeV are interpreted as a constraint on the wino annihilation rate, or alternatively as the minimum core size required such that the wino is not excluded. If there is a thermal wino, H.E.S.S. will be able to probe cores of several kpc, which would begin to cause tension between this dark matter candidate and astrophysical observations/simulations. United States. Department of Energy (Grant DE-SC00012567) United States. Department of Energy (Grant DE-SC0013999) United States. Department of Energy (Grant DE-SCD011090) Simons Foundation (Grant 327942) 2018-12-21T20:37:37Z 2018-12-21T20:37:37Z 2018-12 2018-08 2018-12-18T18:00:54Z Article http://purl.org/eprint/type/JournalArticle 2470-0010 2470-0029 http://hdl.handle.net/1721.1/119830 Rinchiuso, Lucia et al. "Hunting for heavy winos in the Galactic Center." Physical Review D 98, 12 (December 2018): 123014 © 2018 American Physical Society https://orcid.org/0000-0003-3472-7606 https://orcid.org/0000-0001-9699-9047 https://orcid.org/0000-0003-0248-0979 en http://dx.doi.org/10.1103/PhysRevD.98.123014 Physical Review D Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. American Physical Society application/pdf American Physical Society American Physical Society |
| spellingShingle | Rinchiuso, Lucia Moult, Ian Moulin, Emmanuel Baumgart, Matthew Cohen, Timothy Vaidya, Varun Rodd, Nicholas Llewellyn Slatyer, Tracy Robyn Stewart, Iain W Hunting for heavy winos in the Galactic Center |
| title | Hunting for heavy winos in the Galactic Center |
| title_full | Hunting for heavy winos in the Galactic Center |
| title_fullStr | Hunting for heavy winos in the Galactic Center |
| title_full_unstemmed | Hunting for heavy winos in the Galactic Center |
| title_short | Hunting for heavy winos in the Galactic Center |
| title_sort | hunting for heavy winos in the galactic center |
| url | http://hdl.handle.net/1721.1/119830 https://orcid.org/0000-0003-3472-7606 https://orcid.org/0000-0001-9699-9047 https://orcid.org/0000-0003-0248-0979 |
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