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.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2001-12-29T22:51:31Z/2001-12-30T10:49:54Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Prof Koujun Yamashita, 2003, 'Resonance Scattering Effect of Fe-K Emission Lines in anIntracluster Medium', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-bpt220c
