The application of galaxy clusters in constraining cosmological models is currently mostly limited by our uncertain knowledge of scaling relations of observables and cluster mass. Most scaling relation studies are based on X-ray flux limited samples which are biased. In AO10 we proposed to take a new approach with a study of an unbiased volume-limited sample. From this approach and a comparison of both types of samples we will get many new insights into the cluster property statistics. All requested targets have been observed in AO10, but virgul 37 per cent of the observing time has been severly affected by flares. Since we require good data for the full sample, we are requesting the re-observation of 26 clusters for a total of 302 ks not to miss our original goal.
Publication
No observations found associated with the current proposal
Instrument
EPN, OM, RGS1, RGS2, EMOS1, EMOS2
Temporal Coverage
2013-05-02T12:40:33Z/2014-02-20T18:07:03Z
Version
17.56_20190403_1200
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.
European Space Agency, 2015, A New Cosmological Study Approach With A Volume Limited X-Ray Cluster Sample, 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-f2y4i92
