|Title||A YOUNG POOR GALAXY CLUSTER KLEMOLA 44: A COMPARISON WITH CD CLUSTERS|
|Author||Dr TAE FURUSHO|
|Description||We propose to observe a nearby galaxy cluster Klemola 44 with a 20 ksec exposure. One of the recent interesting results found in many cD clusters by Chandra and XMM is a relation between radio and X-ray emission in the cluster core region. Klemola 44 has a radio relic near the cD galaxy, which is a good oppotunity to look into the relation in an early stage of relic evolution. A lower luminosity of central cool components than expected by cooling flow model is now the most interest and problematic topic in cD clusters. The central temperature map and cool emission from galaxies, which are now merging together into a big cD galaxy in this cluster, will give us rich information of the cooling flow problem in comparison with the results of cD clusters.|
|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, 2006-01-05T00:00:00Z, 020446, 17.56_20190403_1200. https://doi.org/10.5270/esa-ylg64pf|