Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408
We present results based on X-ray, optical, and radio observations of the massive galaxy cluster CIZA J0107.7+5408. We find that this system is a post-core-passage, dissociative, binary merger, with the optical galaxy density peaks of each subcluster leading their associated X-ray emission peaks. Th...
| Main Authors: | , , , , , , , , |
|---|---|
| Format: | Journal Article |
| Published: |
Institute of Physics Publishing
2016
|
| Online Access: | http://hdl.handle.net/20.500.11937/74880 |
| _version_ | 1848763399065829376 |
|---|---|
| author | Randall, S. Clarke, T. Van Weeren, R. Intema, Hubertus Dawson, W. Mroczkowski, T. Blanton, E. Bulbul, E. Giacintucci, S. |
| author_facet | Randall, S. Clarke, T. Van Weeren, R. Intema, Hubertus Dawson, W. Mroczkowski, T. Blanton, E. Bulbul, E. Giacintucci, S. |
| author_sort | Randall, S. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | We present results based on X-ray, optical, and radio observations of the massive galaxy cluster CIZA J0107.7+5408. We find that this system is a post-core-passage, dissociative, binary merger, with the optical galaxy density peaks of each subcluster leading their associated X-ray emission peaks. This separation occurs because the diffuse gas experiences ram pressure forces, while the effectively collisionless galaxies (and presumably their associated dark matter (DM) halos) do not. This system contains double-peaked diffuse radio emission, possibly a double radio relic with the relics lying along the merger axis and also leading the X-ray cores. We find evidence for a temperature peak associated with the SW relic, likely created by the same merger shock that is powering the relic radio emission in this region. Thus, this system is a relatively rare, clean example of a dissociative binary merger, which can in principle be used to place constraints on the self-interaction cross-section of DM. Low-frequency radio observations reveal ultra-steep spectrum diffuse radio emission that is not correlated with the X-ray, optical, or high-frequency radio emission. We suggest that these sources are radio phoenixes, which are preexisting non-thermal particle populations that have been re-energized through adiabatic compression by the same merger shocks that power the radio relics. Finally, we place upper limits on inverse Compton emission from the SW radio relic. |
| first_indexed | 2025-11-14T11:02:50Z |
| format | Journal Article |
| id | curtin-20.500.11937-74880 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T11:02:50Z |
| publishDate | 2016 |
| publisher | Institute of Physics Publishing |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-748802019-07-22T03:33:12Z Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408 Randall, S. Clarke, T. Van Weeren, R. Intema, Hubertus Dawson, W. Mroczkowski, T. Blanton, E. Bulbul, E. Giacintucci, S. We present results based on X-ray, optical, and radio observations of the massive galaxy cluster CIZA J0107.7+5408. We find that this system is a post-core-passage, dissociative, binary merger, with the optical galaxy density peaks of each subcluster leading their associated X-ray emission peaks. This separation occurs because the diffuse gas experiences ram pressure forces, while the effectively collisionless galaxies (and presumably their associated dark matter (DM) halos) do not. This system contains double-peaked diffuse radio emission, possibly a double radio relic with the relics lying along the merger axis and also leading the X-ray cores. We find evidence for a temperature peak associated with the SW relic, likely created by the same merger shock that is powering the relic radio emission in this region. Thus, this system is a relatively rare, clean example of a dissociative binary merger, which can in principle be used to place constraints on the self-interaction cross-section of DM. Low-frequency radio observations reveal ultra-steep spectrum diffuse radio emission that is not correlated with the X-ray, optical, or high-frequency radio emission. We suggest that these sources are radio phoenixes, which are preexisting non-thermal particle populations that have been re-energized through adiabatic compression by the same merger shocks that power the radio relics. Finally, we place upper limits on inverse Compton emission from the SW radio relic. 2016 Journal Article http://hdl.handle.net/20.500.11937/74880 10.3847/0004-637X/823/2/94 Institute of Physics Publishing fulltext |
| spellingShingle | Randall, S. Clarke, T. Van Weeren, R. Intema, Hubertus Dawson, W. Mroczkowski, T. Blanton, E. Bulbul, E. Giacintucci, S. Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408 |
| title | Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408 |
| title_full | Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408 |
| title_fullStr | Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408 |
| title_full_unstemmed | Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408 |
| title_short | Multi-wavelength observations of the dissociative merger in the galaxy cluster ciza J0107.7+5408 |
| title_sort | multi-wavelength observations of the dissociative merger in the galaxy cluster ciza j0107.7+5408 |
| url | http://hdl.handle.net/20.500.11937/74880 |