|Title||THE X-RAY PROPERTIES OF HIGH REDSHIFT WEAK-LENSING SELECTED GALAXY CLUSTERS|
|Author||Mr Paul Giles|
|Description||We propose XMM observations (totaling 107 ks) of 6 galaxy clusters in the redshift range 0.3 < z < 0.6 selected in a Subaru weak lensing (WL) survey. This will complete a sample of 8 clusters that will be used to study systematically the X-ray properties of clusters detected independently of their baryonic content. We will investigate biases in cluster selection techniques for high-z clusters, compare the high-z scaling relations of the X-ray properties (e.g. Lx, kT, Mgas, Yx) of WL selected clusters to those of X-ray selected clusters, investigate the evolution of the properties of WL selected clusters from the local to high redshift universe and study their morphology-structure.|
|Publication||Serendipitous UV source catalogues for 10 years of XMM and 5 years of Swift . Yershov, V. N., . Ap&SS . 354-97 . 2014 . 2014Ap&SS.354...97Y ,
|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, 2013-02-04T00:00:00Z, 067466, 17.56_20190403_1200. https://doi.org/10.5270/esa-kj2i2z4|