|Title||The UV to hard X-ray continuum of a Seyfert galaxy scrutinized by XMM and NuSTAR|
|Author||Dr pierre-olivier petrucci|
|Description||We propose to perform a unique XMM-NuSTAR monitoring with 5 repeated observations of 20 ks spaced by a few days of the Seyfert galaxy NGC 4593. This is the best Seyfert candidate to obtain high sensitivity measurements on a day time scale over the entire high energy spectrum. This is an absolute prerequisite 1) to correctly disentangle the different spectral components present in this energy band, and 2) to reveal their complex interdependences and variability behavior. This study will allow us i) to constrain the physical parameters of the Comptonizing corona; ii) to investigate the nature of the soft X-ray excess; iii) to put firm conclusions on the distance, nature and geometry of the reflecting material(s).|
|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, 2016-01-27T23:00:00Z, 074092, 17.56_20190403_1200. https://doi.org/10.5270/esa-qiy17b7|