|Title||X-ray observations of high-redshift quasars|
|Author||Dr Bernd Aschenbach|
|Description||GT-This study aims at a detailed spectral comparison of high-z radio-loud and radio-quiet quasars. The data can provide new insights in quasar formation processes, the evolution and the enigmatic radio-loud-quiet dichotomy. In particular the following questions can be addressed: Do spectral differences between radio-loud and radio-quiet quasars persist to high redshifts? Do radio quiet quasars show intrinsic absorption similar to radio-loud quasars, and do they show spectral evolution? High redshift quasars further serve as back- ground sources to study intervening systems like the intergalactic medium and damped Ly-alpha systems. Is is important to note that XMM provides the last possibility for the foreseeable future to study the X-ray spectra of RQQs.|
|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, 2003-09-11T00:00:00Z, 010306, 17.56_20190403_1200. https://doi.org/10.5270/esa-g2m9t36|