Fossil groups (FGs) present a puzzle to current theories of structure formation.Despite the low number of bright galaxies, their high sigma and high gas T_Xindicate cluster-like potential wells. The measured c200 seem are highindicating early formation epochs, in contradiction with the observed lack oflarge cool cores. There are few FGs with deep X-ray data to date, and theiridiosyncratic characteristics may contribute to enhance these apparentcontradictions. To zero in on their origin and formation mechanisms it isfundamental to increase the number of FGs with good quality X-ray data. Here, wepropose to build the 1st large X-ray sample of bona-fide FGs. True diffuseemission has been verified through 2 Chandra programs. This will allow us to significantly constrain FG.s formation mechanisms.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2010-05-10T14:01:27Z/2010-11-29T07:30:45Z
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, Dr Renato Dupke, 2011, 'Testing the Origin and Evolution of Fossil Groups of Galaxies with XMM-Newton', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-gb3z7kz
