|Title||3C324, the cluster of galaxias with a type-2 QSO|
|Author||Dr Naomi Ota|
|Description||3C324 is a powerful radio galaxy at z=1.2 and the surrounding galaxy cluster has been extensively studied. In particular, X-ray emission detected with ASCA has a hard spectrum described by a superposition of thermal cluster emission and heavily absorbed AGN power-law emission. This is very suggestive of the existence of a type-2 QSO. We propose the 30 ksec XMM observation of 3C324 in order to separate the cluster and the QSO emission. The Iron abundance and the temperature of intracluster gas will constrain the evolution of metallicity and the formation history of clusters in the high-z universe, respectively. Furthermore, measuring the absorption column density of the obscured quasar is important in relation to the composition of the Cosmic X-ray Background.|
|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, 2003-03-08T00:00:00Z, 013604, 17.56_20190403_1200. https://doi.org/10.5270/esa-hh5v2f6|