|Title||The Origin of the Disturbed Cool Core and Filamentary Radio Source in Abell 133|
|Author||Dr Craig Sarazin|
|Description||We will observe A133, a merging cluster with a cooling flow (CF) and a filamentary radio relic. Recently we observed this cluster with Chandra and found a complex central structure. There is an X-ray bright .tongue. extending from the cD to the relic. We suspect that the tongue results from the disruption of the cool core. We will determine the mechanism for the destruction of the core by obtaining the temperature and metalicity distribution. The radio relic may also be a buoyant radio lobe from the cD. We will search for inverse Compton emission from the radio relic, and determine its magnetic field and electron lifetime. We hope to understand the role of central radio sources and cluster mergers in the energetics and disruption of CFs.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2004-02-02T00:00:00Z, 014431, 17.56_20190403_1200. https://doi.org/10.5270/esa-oycr7kd|