|Title||X-RAY SPECTRA OF HIGH REDSHIFT QUASARS|
|Author||Prof SMITA MATHUR|
|Description||We propose to harness both the un-equalled sensitivity of XMM and its broad energy band to systematically study a sample of 9 high redshift(z > 4) quasars, the most luminous, youngest and least studied objects known(4 new observations). XMM can determine accurately both the absorption column density and the X-ray spectral shape allowing us to resolve intriguing, outstanding questions such as: Is the apparent difference between the X-ray spectra of high-redshift radio-loud and radio-quiet quasars real? If so, is it explained by intrinsic absorption or by different evolution of the X-ray spectrum with redshift? What constraints can we place on the X-ray spectral evolution with redshift and-or luminosity for each class? What limits can we put on intervening Damped Ly-alpha systems?|
|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, 2006-01-27T00:00:00Z, 020346, 17.56_20190403_1200. https://doi.org/10.5270/esa-yriv8c2|