|Title||The X-ray spectrum of the luminous quasar RBS 315|
|Author||Dr Georg Lamer|
|Description||With log(lx)=47.0 RBS315 is one of the most X-ray luminous quasars known. Despite its redshift of z=2.69 it is bright enough in X-rays to obtain a high quality spectrum with EPIC. We propose to observe RBS315 for 20 ksec in order to obtain a high SNR X-ray spectrum spanning a source frame energy range of 0.7-40 keV. Important spectral features as the 6.4 keV iron fluorescence line, the iron 7.11 keV absorption edge and the Compton reflection hump are redshifted to favourable energies. We intend to measure the EW, energy, and shape of the fluorescence line and measure the relative contributions of jet emission and nuclear emission to the X-ray spectrum. We will also investigate possible intrinsic absorption of the X-ray source.|
|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, 2004-09-13T00:00:00Z, 015018, 17.56_20190403_1200. https://doi.org/10.5270/esa-xvla62k|