|Title||A broad iron-K emission line and an outflow at z virgul 1|
|Author||Dr Emanuele Nardini|
|Description||We propose to observe for a full XMM-Newton orbit (virgul120 ks) the lensed quasar B 1152+199 (z = 1.019). The flux magnification will make it possible to study in detail the central regions of this quasar, where two previous Chandra snapshots (of 16 and 8 ks) suggest the presence of a broad iron line from the accretion disc and possible absorption. Such features, almost ubiquitous in the local Universe, are still elusive at moderate-high redshift due to the low data quality usually available, in spite of their important implications in terms of supermassive black hole accretion history, cosmic X-ray background, and feedback. The new spectrum will allow the detection of any emission and-or absorption line down to an equivalent width of about 100 eV.|
|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, 2019-01-30T23:00:00Z, 080468, 17.56_20190403_1200. https://doi.org/10.5270/esa-2mml5ph|