A 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP Line
Galaxy clusters can efficiently convert axion-like particles (ALPs) to photons. We propose that the recently claimed detection of a 3.55--3.57 keV line in the stacked spectra of a large number of galaxy clusters and the Andromeda galaxy may originate from the decay of either a scalar or fermionic $7...
| Main Authors: | , , , |
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| Format: | Journal article |
| Language: | English |
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American Physical Society
2014
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| _version_ | 1797071102678138880 |
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| author | Cicoli, M Conlon, J Marsh, M Rummel, M |
| author_facet | Cicoli, M Conlon, J Marsh, M Rummel, M |
| author_sort | Cicoli, M |
| collection | OXFORD |
| description | Galaxy clusters can efficiently convert axion-like particles (ALPs) to photons. We propose that the recently claimed detection of a 3.55--3.57 keV line in the stacked spectra of a large number of galaxy clusters and the Andromeda galaxy may originate from the decay of either a scalar or fermionic $7.1$ keV dark matter species into an axion-like particle (ALP) of mass $m_{a} \lesssim 6\cdot 10^{-11}~{\rm eV}$, which subsequently converts to a photon in the cluster magnetic field. In contrast to models in which the photon line arises directly from dark matter decay or annihilation, this can explain the anomalous line strength in the Perseus cluster. As axion-photon conversion scales as $B^2$ and cool core clusters have high central magnetic fields, this model can also explains the observed peaking of the line emission in the cool cores of the Perseus, Ophiuchus and Centaurus clusters, as opposed to the much larger dark matter halos. We describe distinctive predictions of this scenario for future observations. |
| first_indexed | 2024-03-06T22:48:26Z |
| format | Journal article |
| id | oxford-uuid:5dfcfcca-3ba8-4727-8726-535b8f7f8c5c |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T22:48:26Z |
| publishDate | 2014 |
| publisher | American Physical Society |
| record_format | dspace |
| spelling | oxford-uuid:5dfcfcca-3ba8-4727-8726-535b8f7f8c5c2022-03-26T17:37:40ZA 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP LineJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:5dfcfcca-3ba8-4727-8726-535b8f7f8c5cEnglishSymplectic Elements at OxfordAmerican Physical Society2014Cicoli, MConlon, JMarsh, MRummel, MGalaxy clusters can efficiently convert axion-like particles (ALPs) to photons. We propose that the recently claimed detection of a 3.55--3.57 keV line in the stacked spectra of a large number of galaxy clusters and the Andromeda galaxy may originate from the decay of either a scalar or fermionic $7.1$ keV dark matter species into an axion-like particle (ALP) of mass $m_{a} \lesssim 6\cdot 10^{-11}~{\rm eV}$, which subsequently converts to a photon in the cluster magnetic field. In contrast to models in which the photon line arises directly from dark matter decay or annihilation, this can explain the anomalous line strength in the Perseus cluster. As axion-photon conversion scales as $B^2$ and cool core clusters have high central magnetic fields, this model can also explains the observed peaking of the line emission in the cool cores of the Perseus, Ophiuchus and Centaurus clusters, as opposed to the much larger dark matter halos. We describe distinctive predictions of this scenario for future observations. |
| spellingShingle | Cicoli, M Conlon, J Marsh, M Rummel, M A 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP Line |
| title | A 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP Line |
| title_full | A 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP Line |
| title_fullStr | A 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP Line |
| title_full_unstemmed | A 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP Line |
| title_short | A 3.55 keV Photon Line and its Morphology from a 3.55 keV ALP Line |
| title_sort | 3 55 kev photon line and its morphology from a 3 55 kev alp line |
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