|Title||Searching First Robust Evidence of Charge Exchange Emission from the Cygnus Loop|
|Author||Dr Hiroyuki Uchida|
|Description||We propose to observe a southwestern knot (SW-K) in the Cygnus Loop. The aim is to find first robust evidence for charge exchange (CX) emission from SNRs. Our comprehensive SUzaku XIS studies have found a possible sign of CX. However, due to the lack of the energy resolution of the XIS, we cannot resolve them clearly and thus cannot exclude other possibilities from their spectra. The SW-K is one of the brightest and the most compact region among them. Our simulation shows that the RGS can clearly divide the O Hea and the Ne Hea triplets into three lines. Their forbidden-to-resonance ratios are useful to find conclusive evidence for the existence of CX emission from the Cygnus Loop. A 100 ks observation is required for this purpose.|
|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, 2013-06-01T00:00:00Z, 069340, 17.56_20190403_1200. https://doi.org/10.5270/esa-mbcwg9r|