|Title||THE PHYSICS OF BALQSO WINDS|
|Author||Prof FRED HAMANN|
|Description||Recent X-ray observations of BALQSOs reveal absorption column densities that are 2 or more orders of magnitude larger than previous estimates based on the UV BALs. Part of this discrepancy can be explained by saturation in the BALs. However, the relationship between the UV and X-ray absorbers remains unknown; simply attributing the huge X-ray column densities to outflowing BAL gas would have profound implications for the wind properties. We have already obtained HST spectra of several BALQSOs that provide rare measurements of weak lines (less susceptible to saturation). We now propose XMM observations of three of these targets. The combined data set will provide the best available constraints on the UV-X-ray absorber relationship and the overall outflow-absorber properties.|
|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, 2005-08-10T00:00:00Z, 020002, 17.56_20190403_1200. https://doi.org/10.5270/esa-bhovh0q|