|Title||REVEALING THE HIGH VELOCITY OUTFLOW IN PG 1211+143|
|Author||Dr JAMES REEVES|
|Description||We propose a 150 ksec ACIS-S-LETGS observation of the proto-type Big Blue Bump quasar, PG 1211+143. In our recent XMM-Newton observation, we found evidence for one of the most extreme X-ray outflows yet observed in an AGN. Indeed the outflow velocity (0.1c) and kinetic output are similar to that seen in the most powerful BAL quasars. We will utilize the high spectral resolution, bandpass and sensitivity of the ACIS-S-LETGS combination to measure the outflow velocities of the highly ionized absorption lines of N, O, Ne, Mg, Si, and S in the soft X-ray band, to fully understand the dynamics of this extraordinary outflow. We also request a simultaneous, 50 ksec XMM-Newton observation to detect the blue shifted Fe XXV and Fe XXVI K-shell lines, with the EPIC detectors above 6 keV.|
|Publication||No observations found associated with the current proposal|
|Instrument||EPN, RGS1, OM, RGS2, EMOS1, EMOS2|
|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, 2005-07-27T00:00:00Z, 020802, 17.56_20190403_1200. https://doi.org/10.5270/esa-lik86dw|