|Title||Nailing Down the Population of Intrinsically X-ray Weak BAL Quasars|
|Author||Prof William Brandt|
|Description||There are few intrinsically X-ray weak AGNs reliably identified to date. Such systems may exist preferentially in broad absorption line (BAL) quasars, where it is challenging to ascribe the observed X-ray weakness to absorption vs. intrinsic X-ray weakness. We selected two candidates for intrinsically X-ray weak BAL quasars from the well-defined z virgul 2 LBQS BAL quasar sample. These objects are only weakly detected in the current Chandra observations, hampering rigorous conclusions about their nature. We thus propose 85 ks XMM-Newton observations for the two candidates, in order to confirm their intrinsically X-ray weak nature, obtain the fraction of intrinsically X-ray weak BAL quasars, and probe the underlying physics.|
|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, 2022-02-24T00:00:00Z, 086053, 18.02_20200221_1200. https://doi.org/10.5270/esa-[xxxxxxx]|