|Title||XMM Observations of two best studied Clusters of Galaxies at z=0.8 SSC_16|
|Author||Dr Michael Watson|
|Description||GT-There are six X-ray luminous clusters in the EMSS at z above 0.5: MS1054-03 and MS1137+66; z=0.83 and 0.78 respectively. They are among the very few high redshift clusters known which have been extensively studied in the optical and in the X-rays. Here we propose to observe them with the aim of measuring X-ray temperature and iron abundance. Only with the high resolution + troughput of XMM it will be possible to perform spatially resolved spectroscopy and to measure the Fe-H abundances at redshifts this high. We will estimate the metallicity and gravitational mass for the two distant clusters and compare these quantities to nearby clusters with similarly high X-ray luminosities (Lx larger than 10E45) and well determined cluster temperatures.|
|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, 2002-09-13T00:00:00Z, 009480, 17.56_20190403_1200. https://doi.org/10.5270/esa-pksbmhd|