|Title||X-ray Counterparts of Be Gamma-ray Binary Candidates|
|Author||Dr M. Virginia McSwain|
|Description||The AGILE and Fermi missions have detected hundreds of unidentified GeV sources in the Galactic plane, but only a handful have been correlated with X-ray or optical counterparts. Several of these are high mass X-ray binaries that also exhibit MeV, GeV, and-or TeV emission, leading to a new class of "gamma-ray binaries". More than half of all HMXB contain Be stars, and likewise most of the known gamma-ray binaries are Be star systems. We have identified three new Be stars that may be associated with GeV point sources, and we propose XMM-Newton observations to measure the position, flux, and spectral properties of the X-ray counterparts. Our modest time request will help identify several unknown GeV point sources, potentially doubling the number of known Be-gamma-ray binaries.|
|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, 2013-04-18T00:00:00Z, 067232, 17.56_20190403_1200. https://doi.org/10.5270/esa-c4zgkes|