|Title||THE COOLEST CORONA IN THE EDDINGTON-LIMITED AGN ARK 564|
|Author||Dr Erin Kara|
|Description||Ark 564 is a luminous accreting supermassive black hole that has revealed several extraordinary qualities in soft X-rays: it is the brightest NLS1 from 0.3-10 keV, is one of the most highly variable AGN, has a very steep spectrum and strong soft excess. In NuSTAR AO1, we were awarded 200 ks to study this source above 20 keV for the first time, and discovered that Ark 564 is as exceptional in hard X-rays as it is in soft. Ark 564 has a coronal temperature of 15 2 keV, one of the lowest ever observed, and also shows an iron K line complex that is so highly ionised that it resembles more closely a black hole binary than an AGN. We now propose for an additional 500 ks of NuSTAR observations, simultaneous with 200 ks of XMM-Newton time and 100 ks of NICER time.|
|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, 2019-12-21T23:00:00Z, 083054, 17.56_20190403_1200. https://doi.org/10.5270/esa-9kz85e8|