|Title||Spectro-Imaging of Dust Scattering Haloes|
|Author||Dr Bernd Aschenbach|
|Description||Bright and absorbed galactic X-ray sources are surrounded by haloes of radiation scattered on interstellar dust grains. It is proposed to study the physical and chemical properties of these grains, in particular whether or not grains have silicate cores surrounded by organic mantles. The refractive index of both and therefore the scattering cross sections are substantially different. Therfore, the shape of a spectrally resolved halo could be dominated either by one component or the other. Cyg X-2 and GX 339-4 have been selected because they have bright haloes but are not too absorbed in order to get sufficient intensity even at lower energies. Another observation of GX 339-4 in timing mode (Wilms et al.) is devoted to the properties of the central source only.|
|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, 2005-04-20T00:00:00Z, 011136, 17.56_20190403_1200. https://doi.org/10.5270/esa-k6kqw74|