|Title||The Fe line diagnostic of the nuclear source in the prototype ULIG Arp220|
|Author||Prof DAVID SANDERS|
|Description||We propose a 90ks XMM-Newton-EPIC observation of the Ultra-Luminous Infrared Galaxy Arp220,the nearest ULIG. Based on ASCA and BeppoSAX observations,if an AGN were the major evergy source in this object,it must be Compton-thick. A 50ks Chandra observation has located a faint hard X-ray source at one of the double nuclei, and the spectrum hinted at the presence of an iron K-line. The primary aim of this proposal is to obtain a high quality iron K-line spectrum with the EPIC cameras in order to determine the origin of the hard X-ray emission, which we believe will provide the ultimate test as to whether an AGN powers the enormous infrared luminosity in this "prototype" ULIG, as well as have important implications for interpreting the X-ray emission from all ULIGs.|
|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, 2006-07-08T00:00:00Z, 020551, 17.56_20190403_1200. https://doi.org/10.5270/esa-y42am9w|