|Title||Hyperluminous IRAS galaxies: solving the AGN-starburst mystery with XMM|
|Author||Dr Kirpal Nandra|
|Description||There is still substantial debate over whether luminous infrared galaxies are powered primarily by AGN or star-formation. Although both processes are clearly involved, and may be intimately related, the heavy obscuration in these sources makes disentangling the components very difficult. Hard X-rays can penetrate this obscuration and reveal the hidden AGN, if present. With sufficiantly sensitive observations, it should even be possible to detect the X-ray emission expected from the star-formation processes, even if there is no accreting supermassive black hole. XMM observations therefore have the potential solve this long-standing mystery. Here we propose to observe 8 hyperluminous infrared galaxiues - the most extreme examples - which form part of an unbiased sample.|
|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, 2004-09-11T00:00:00Z, 014757, 17.56_20190403_1200. https://doi.org/10.5270/esa-tcslm4j|