|Title||Mapping the Inner Accretion Disk Wind in the Quasar PDS 456|
|Author||Dr James Reeves|
|Description||PDS 456 is the most luminous nearby AGN, more typical of quasars at high redshift. A previous 40ks XMM-Newton (2001) observation revealed deep, highly ionised absorption at iron K and at 1 keV in the RGS spectrum. Subsequent Suzaku observations resolved the powerful ionised outflow, moving at 0.25c and revealed a direct response of the iron K absorption to a decrease in the ionising flux. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a series of 5x100ks XMM-Newton observations. From the timescale of the absorber variability we will probe the inner structure of the quasar wind, on scales of 10s-100s of Rg from the black hole and determine the intrinsic mechanism for the rapid variability in PDS 456.|
|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, 2015-03-26T23:00:00Z, 072101, 17.56_20190403_1200. https://doi.org/10.5270/esa-qsixpuj|