|Title||XMM Observations of Low Mass Groups|
|Author||Dr David Davis|
|Description||ASCA and ROSAT observations show that many groups of galaxies contain diffuse hot gas and that the metalicity of this gas quickly decreases with decreasing gas temperature. This trend is thought to occur because winds from early ellipticals cannot be contained by low mass groups. While high temperature, high metalicity groups are currently included in the XMM GTO program the groups with the lowest masses (lowest temperature and abundances) are not. These low mass groups may be important contributors of metals to the intergalactic medium. We propose to use the excellent spatial and spectral capabilities of XMM to determine the enrichement history of the hot gas and thus infer the amount of material which may have been ejected from poor groups and thus enriching the IGM|
|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, 2003-05-16T00:00:00Z, 002234, 17.56_20190403_1200. https://doi.org/10.5270/esa-1o1blgf|