|Title||The X-ray nuclei of FRII radio galaxies: unification and accretion modes|
|Author||Dr Martin Hardcastle|
|Description||We have recently shown that a population of powerful radio galaxies, the low-excitation FRII radio galaxies, appears to have no accretion-related nuclear X-ray emission, despite having high-luminosity radio jets: plausibly these objects are accreting via a different, radiatively inefficient accretion mode compared to the better understood narrow-line radio galaxies and quasars. This picture is consistent with other information from the optical and infrared bands, but the crucial X-ray constraints come from a small and inhomogenous sample. We propose observations of a sample of low-excitation and narrow-line radio galaxies which will greatly increase our sample size and allow us to make definitive statements about the nature of the accretion mode in these objects.|
|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, 2010-04-30T00:00:00Z, 055176, 17.56_20190403_1200. https://doi.org/10.5270/esa-zefr4sn|