|Title||Resonance Scattering Effect of Fe-K Emission Lines in anIntracluster Medium|
|Author||Prof Koujun Yamashita|
|Description||It is noticeable that the optical depth of Fe-Ka resonance lines is estimated to be larger than unity in an intracluster medium due to the resonance scattering effect. Therefore the intensity of Fe-Ka lines is suppressed in the central core region and enhanced in the outer envelope. The intensity ratios of Fe-Ka to Kb and He-like to H-like Fe-Ka are good indicators to derive the optical depth of Fe-Ka by means of the difference of the resonance scattering cross section. Our objectives are to correctly determine the Fe abundance and to derive the absolute scale of a cluster. We propose the observation of A1650 (z=0.0845) which is isothermal spherical symmetric with the angular size of 30. fit in the EPIC field of view and the plasma temperature of 6.1keV.|
|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, 2003-01-25T00:00:00Z, 009320, 17.56_20190403_1200. https://doi.org/10.5270/esa-bpt220c|