|Title||Classification of a New Type of X-ray Weak Quasar|
|Author||Prof Bin Luo|
|Description||Luminous X-ray emission is an ubiquitous property of quasars. Small populations of type 1 quasars have displayed weak X-ray emission, generally due to absorption or variability effects. We have discovered several X-ray weak SDSS quasars that do not fit easily into any of the known categories. We propose to obtain 30-50 ks XMM-Newton observations for three of these exceptional X-ray weak quasars. We will determine reliably whether there is X-ray variability or X-ray absorption, and then classify the possible causes for their observed X-ray weakness. Understanding this new type of X-ray weak quasar might provide new insights into the X-ray corona and its environment. It will also allow us to constrain the missed fraction of SMBH growth in extragalactic X-ray surveys.|
|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, 2022-05-05T00:00:00Z, 086126, 19.16_20210326_1200. https://doi.org/esa-[xxxxxxx]|