|Title||XMM observations of HESSJ1804-216: a clue to the PSR1800-21:G8.7-0.1 association|
|Author||Dr Gerd Puehlhofer|
|Description||The TeV instrument H.E.S.S. discovered during a survey of the Galactic plane three sources close to highly energetic pulsars. It was hence suggested that these gamma-ray sources are counterparts of pulsar wind nebulae (PWN). Indeed, in one of these cases the PWN has been well studied with XMM-Newton, which allowed a firm identification of the TeV source with the PWN. With this proposal, we want to use XMM-Newton to identify the X-ray counterpart of HESS J1804-216. This TeV source can also most likely be explained as emission from a PWN, but so far this PWN around PSR B1800-21 has not been detected in any other waveband. The PWN detection may also hold the clue for the so far not firmly established association of PSR B1800-21 to the supernova remnant G8.7-0.1.|
|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, 2008-03-23T00:00:00Z, 040575, 17.56_20190403_1200. https://doi.org/10.5270/esa-7hdfywh|