|Title||Unveiling the Xray faint intermediate polars-source of the Galactic Ridge X-rays|
|Author||Dr Hauke Worpel|
|Description||The poorly-understood Galactic Ridge X-ray Emission (GRXE) is an X-ray background concentrated around the Galactic plane, primarily composed of difficult to resolve discrete sources. The most promising candidates for its origin above a few keV are the intermediate polars (IPs), a class of magnetic cataclysmic variables (CVs), consisting of a strongly magnetic white dwarf and a Roche-lobe filling companion. Most of the 49 confirmed IPs are X-ray bright (L_X approx 10^33 erg-s) but there may be a more numerous undiscovered population of fainter (L_X approx 10^31 erg-s) IPs. We propose to observe 13 underluminous IP candidates to confirm their nature as IPs, to search for the underluminous IP population, detect spin period|
|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, 2019-05-14T22:00:00Z, 080411, 17.56_20190403_1200. https://doi.org/10.5270/esa-jmefv2o|