|Title||Enrichment and cooling in the Centaurus cluster|
|Author||Dr Jeremy Sanders|
|Description||We propose a deep 140ks observation of the Centaurus cluster, one of the brightest clusters. It presents an ideal opportunity to study the physics of enrichment in great detail, given its very high metallicity, its proximity, its cool temperature, and luminosity. Our Chandra results show that there is the same ratio of Type Ia to II SN abundances over the inner 60kpc, which is of great importance to understanding cluster enrichment. We will investigate in detail whether this is replicated in the outer regions, and relate this to enrichment mechanisms. The observation is very well matched to XMM. We will study the merger between the two subgroups. The cluster also shows a very wide range in temperature, making it ideal to limit the amount cooling out of the X-ray band.|
|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, 2007-08-23T00:00:00Z, 040620, 17.56_20190403_1200. https://doi.org/10.5270/esa-o2dylmk|