|Title||The Physics of Cooling Flow Clusters with Central Radio Sources|
|Author||Dr Craig Sarazin|
|Description||Central galaxies in rich clusters are the sites of cluster cooling flows, with large masses of gas cooling through part of the X-ray band. Many of these galaxies host powerful radio sources. These sources can displace and compress the X-ray gas leading to enhanced cooling and star formation. We propose observations of two bright cooling flows (A1367 & A2147) with radio sources that will exploit the large collecting area and spectral resolution of XMM-Newton. We will constrain the source of additional pressure in radio "holes" in the X-ray emission needed to support overlying shells of X-ray gas. We will address the problem of the lack of kT less than 1-2 keV gas in cooling flows by searching for abundance inhomogeneities, heating from the radio source, and excess absorption.|
|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, 2007-02-19T00:00:00Z, 030035, 17.56_20190403_1200. https://doi.org/10.5270/esa-3e142wn|