RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER
The recent discovery of the unidentified emission line at 3.5 keV in galaxies and clusters has attracted great interest from the community. As the origin of the line remains uncertain, we study the surface brightness distribution of the line in the Perseus cluster since that information can be used...
| Main Authors: | , , , , , , , , , , , , , |
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| Other Authors: | |
| Format: | Article |
| Language: | en_US |
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IOP Publishing
2017
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| Online Access: | http://hdl.handle.net/1721.1/108040 https://orcid.org/0000-0001-5226-8349 |
| _version_ | 1811081553694949376 |
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| author | Franse, Jeroen Foster, Adam Boyarsky, Alexey Markevitch, Maxim Iakubovskyi, Dmytro Loewenstein, Mike Miller, Eric Randall, Scott W. Ruchayskiy, Oleg Smith, Randall K. Bulbul, Gul E Bautz, Mark McDonald, Michael A. Miller, Eric D |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Franse, Jeroen Foster, Adam Boyarsky, Alexey Markevitch, Maxim Iakubovskyi, Dmytro Loewenstein, Mike Miller, Eric Randall, Scott W. Ruchayskiy, Oleg Smith, Randall K. Bulbul, Gul E Bautz, Mark McDonald, Michael A. Miller, Eric D |
| author_sort | Franse, Jeroen |
| collection | MIT |
| description | The recent discovery of the unidentified emission line at 3.5 keV in galaxies and clusters has attracted great interest from the community. As the origin of the line remains uncertain, we study the surface brightness distribution of the line in the Perseus cluster since that information can be used to identify its origin. We examine the flux distribution of the 3.5 keV line in the deep Suzaku observations of the Perseus cluster in detail. The 3.5 keV line is observed in three concentric annuli in the central observations, although the observations of the outskirts of the cluster did not reveal such a signal. We establish that these detections and the upper limits from the non-detections are consistent with a dark matter decay origin. However, absence of positive detection in the outskirts is also consistent with some unknown astrophysical origin of the line in the dense gas of the Perseus core, as well as with a dark matter origin with a steeper dependence on mass than the dark matter decay. We also comment on several recently published analyses of the 3.5 keV line. |
| first_indexed | 2024-09-23T11:48:23Z |
| format | Article |
| id | mit-1721.1/108040 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T11:48:23Z |
| publishDate | 2017 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/1080402022-09-27T22:03:17Z RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R 200 IN THE PERSEUS CLUSTER Franse, Jeroen Foster, Adam Boyarsky, Alexey Markevitch, Maxim Iakubovskyi, Dmytro Loewenstein, Mike Miller, Eric Randall, Scott W. Ruchayskiy, Oleg Smith, Randall K. Bulbul, Gul E Bautz, Mark McDonald, Michael A. Miller, Eric D Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Bulbul, Gul E Bautz, Mark McDonald, Michael A. Miller, Eric D The recent discovery of the unidentified emission line at 3.5 keV in galaxies and clusters has attracted great interest from the community. As the origin of the line remains uncertain, we study the surface brightness distribution of the line in the Perseus cluster since that information can be used to identify its origin. We examine the flux distribution of the 3.5 keV line in the deep Suzaku observations of the Perseus cluster in detail. The 3.5 keV line is observed in three concentric annuli in the central observations, although the observations of the outskirts of the cluster did not reveal such a signal. We establish that these detections and the upper limits from the non-detections are consistent with a dark matter decay origin. However, absence of positive detection in the outskirts is also consistent with some unknown astrophysical origin of the line in the dense gas of the Perseus core, as well as with a dark matter origin with a steeper dependence on mass than the dark matter decay. We also comment on several recently published analyses of the 3.5 keV line. United States. National Aeronautics and Space Administration (Contracts NNX14AF78G and NNX123AE77G) 2017-04-11T13:55:33Z 2017-04-11T13:55:33Z 2016-10 2016-06 Article http://purl.org/eprint/type/JournalArticle 1538-4357 0004-637X http://hdl.handle.net/1721.1/108040 Franse, Jeroen et al. “RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R 200 IN THE PERSEUS CLUSTER.” The Astrophysical Journal 829.2 (2016): 124. © 2016 The American Astronomical Society https://orcid.org/0000-0001-5226-8349 en_US http://dx.doi.org/10.3847/0004-637X/829/2/124 Astrophysical Journal 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. application/pdf IOP Publishing IOP Publishing |
| spellingShingle | Franse, Jeroen Foster, Adam Boyarsky, Alexey Markevitch, Maxim Iakubovskyi, Dmytro Loewenstein, Mike Miller, Eric Randall, Scott W. Ruchayskiy, Oleg Smith, Randall K. Bulbul, Gul E Bautz, Mark McDonald, Michael A. Miller, Eric D RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER |
| title | RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER |
| title_full | RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER |
| title_fullStr | RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER |
| title_full_unstemmed | RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER |
| title_short | RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R[subscript 200] IN THE PERSEUS CLUSTER |
| title_sort | radial profile of the 3 5 kev line out to r subscript 200 in the perseus cluster |
| url | http://hdl.handle.net/1721.1/108040 https://orcid.org/0000-0001-5226-8349 |
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