|Title||The 6.7 keV-line emission in the Galactic Centre|
|Author||Dr Masaaki Sakano|
|Description||The Galactic Centre Region emits a strong 6.7-keV line attributable to Ka emission of He-like iron, of which the origin has remained a puzzle since its discovery. Arguably, recent Chandra results imply that the line is produced in a hot extended plasma. However, we have shown that the line has a relatively smooth, circularly symmetric distribution centred on Sgr A* and a surface brightness which falls off with radius as 1-r over the range r=3.-12. This mirrors the distribution of the stellar population and adds strong support to the hypothesis that the 6.7-keV line originates in the summed emission of faint point sources. Here we propose to measure the surface brightness distribution of the 6.7-keV line out to a radius of virgul35. as a test of the competing scenarios for its origin.|
|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, 2009-04-11T00:00:00Z, 050587, 17.56_20190403_1200. https://doi.org/10.5270/esa-20kxbih|