|Title||The 1st systematic XR Study of extreme accretion on supermassive BH with NU+XM|
|Author||Prof Claudio Ricci|
|Description||Super-Eddington accretion periods are expected to be extremely important to explain the fast growth of the first supermassive black holes. However,among all accretion modes, this phase is still the least understood one,and it is still largely debated what are the physical properties of the accretion flow and of the X-ray source at very high accretion rates. We propose here a systematic broad-band X-ray study of super-Eddington AGN at z<0.1 by simultaneously observing three sources with NuSTAR and XMM.These three AGN have the highest Eddington ratios in the SEAMBHs sample, which contains exclusively objects with black hole masses estimated from reverberation mapping, making the Eddington ratio estimates extremely reliable.|
|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, 2021-04-24T00:00:00Z, 085206, 18.02_20200221_1200. https://doi.org/10.5270/esa-[xxxxxxx]|