|Title||The concentration-mass relation in galaxy clusters|
|Author||Dr Edward Lloyd-Davies|
|Description||The concentration of the dark matter haloes of galaxy clusters is related through their formation times to the power spectrum of perturbations from which they formed. Measurements of the variation of concentration with mass therefore provide interesting constraints on cosmological models. However presently accepted observations of XMM will be able to accurately measure concentrations over a limited mass range of about 10^14-10^15 solar masses. We propose to supplement this with observations of galaxy groups in the range 10^13-10^14 solar masses in order to more precisely measure the slope and possible curvature of the relation. Constraints on individual formation times can be correlated with system properties to probe other physical processes.|
|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, 2004-11-01T00:00:00Z, 015127, 17.56_20190403_1200. https://doi.org/10.5270/esa-q43jdm7|