|Title||Revealing the X-ray counterpart of the gamma-ray binary candidate HD 215227|
|Author||Mr Pere Munar Adrover|
|Description||Only 7 Galactic binary systems displaying GeV-TeV emission are known, and the physical properties of these powerful accelerators are still under discussion. The Be star HD 215227, displaying a photometric period of 60 days, has been suggested to be a new gamma-ray binary, although no X-ray counterpart has been found in the limited archival data available. Our recent optical spectroscopic results unveil that HD 215227 is indeed a binary system, and the orbital ephemeris have allowed us to predict the epochs of expected enhanced X-ray emission. We request a 10-ks observation 0.3 orbital phases after periastron to discover the X-ray counterpart and unveil the non-thermal nature of the putative X-ray source. We are conducting multi-wavelength studies of the source.|
|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, 2014-06-19T00:00:00Z, 072361, 17.56_20190403_1200. https://doi.org/10.5270/esa-vj35trk|