|Title||Exotic Quasars at the Highest Redshift|
|Author||Dr Bradford Snios|
|Description||Recent discoveries of high-redshift quasars have provided new opportunities to investigate fundamental properties of the early Universe. X-ray observations of this quasar population are especially important for studies of black hole formation and the initial stages of feedback. We propose observations of two high-z radio-loud quasars with X-ray properties that represent the extremes of comparable sources to perform the following: (1) establish the formation of a Compton thick absorber at high redshift, (2) investigate the accretion disk structure via Fe K intensity and broadening. These results will provide an invaluable perspective on X-ray emission from exotic systems and establish the diversity in X-ray emission from young radio sources at the highest redshifts.|
|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, 2021-07-23T00:00:00Z, 086240, 18.02_20200221_1200. https://doi.org/10.5270/esa-[xxxxxxx]|