|Title||The Extreme Hard Excess and Black Hole Spin of IRAS 13197-1627|
|Author||Dr Dominic Walton|
|Description||The nearby type 1.8 Seyfert galaxy IRAS 13197-1627 shows evidence for some of the strongest accretion disk reflection observed among local, Compton-thin AGN. This indicates an extreme accretion geometry in which the intrinsic continuum emission experiences strong gravitational light bending, resulting in an X-ray spectrum dominated by reflection from the inner accretion disk. We request a coordinated broadband X-ray observation of this remarkable source with XMM and NuSTAR. This will enable us to robustly confirm the extreme reflection, and utilize the full potential of the latest models to measure the black hole spin and constrain the coronal geometry, self-consistently accounting for both the relative strength and the profile of the reflected emission.|
|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, 2017-02-04T23:00:00Z, 076322, 17.56_20190403_1200. https://doi.org/10.5270/esa-q2o60ms|