|Title||Exploring cosmic-ray acceleration environment in the SNR CTB37B|
|Author||Ms Ryoko Nakamura|
|Description||Although cosmic rays are accelerated at the shock front of supernova remnants (SNRs), condition for the particle accelation to occur is poorly understood. One of the ways to resolve this problem is to investigate thermal X-ray emission associated with the acceleration site, because the thermal emission provides us the information of the condistions. We propose XMM-Newton of the SNR CTB37B which has thermal, non-thermal X-ray and TeV I?-ray emission. Suzaku and Chandra observations could not determine the parameters of the thermal plasma because of the contamination of a point source and of statistical limitation. Only good spatial resolution and large effective area of XMM-Newton enable us to investigate the thermal X-ray emission.|
|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, 2011-04-24T00:00:00Z, 060602, 17.56_20190403_1200. https://doi.org/10.5270/esa-9k5dyp9|