|Title||The Cosmological Parameters for the redshift range from 5.6 to 7.0|
|Author||Dr Norbert Schartel|
|Description||With the paper "A Hubble Diagram for Quasars" Risaliti and Lusso (2015) established quasars as a kind of standard candles to measure cosmological parameters. This method is of utmost importance as it allows to measure the cosmological parameters for different redshift ranges and to test for an evolution of the parameters over cosmological time. We propose to observe 131 quasars at a redshift higher than 5.6, i.e. nearly all known such quasars (Banados et al., 2016) not yet observed in X-ray. The aim is to measure the cosmological parameters with high precision in the redshift range from 5.6 to 7.0 for the first time. This redshift range is not accessible with any other method, e.g. supernovae, clusters of galaxies, microwave back ground or baryon|
|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, 2020-01-03T23:00:00Z, 082056, 17.56_20190403_1200. https://doi.org/10.5270/esa-1hg3pyi|