|Title||Connecting compact ultra-fast outflows with galaxy-wide AGN-driven winds|
|Author||Dr Mirko Krumpe|
|Description||We propose a deep 175 ks observation of the close-by, X-ray bright AGN HE1353-1917. MUSE, a ground-breaking new IFU spectrograph on the VLT, provided unprecedented 3D coverage of the object. The optical data show the strongest evidence of a kpc-scale outflow from an AGN in a well-defined sample of luminous nearby AGN. The search for signs of X-ray outflows (ultra-fast outflows and-or warm absorbers) will identify whether or not these (sub)parsec-scale X-ray outflows of the AGN can be connected to the kilo-parsec optical phenomena. Using both X-ray and existing IFU data will enable us to connect the velocity profile as a function of distance from the center. The results will be used to constrain if the outflows are momentum- or energy-driven.|
|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, 2018-08-30T22:00:00Z, 080351, 17.56_20190403_1200. https://doi.org/10.5270/esa-t2swk7u|