|Title||A hunt for X-ray absorbed Narrow Line Seyfert 1s using the FeII-Hbeta ratio|
|Author||Dr Enrico Piconcelli|
|Description||We propose to observe a sample of four Narrow Line Seyfert 1 galaxies with strong Fe II emission (FeNLS1s) for a total allocation time of 115 ks. The goal of this proposal is to test how common is the spectral hard X-ray (Evirgul7-8 keV) absorption feature in FeNLS1s, recently observed in two objects of this class. This feature appears as a clear signature of dense matter outflowing from the nucleus. If our optically-based criterion (i.e. Fe II4570-Hbeta higher than 1.5) would be efficient in selecting objects with deep sharp X-ray edges, the origin of this feature in outflowing clouds would be supported. A frequent occurrence of this spectral drop will therefore provide clues of an intimate link between NLS1s and BAL QSOs phenomena.|
|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, 2008-01-10T00:00:00Z, 030091, 17.56_20190403_1200. https://doi.org/10.5270/esa-24k3f4t|