|Title||Identification of GRLB candidates|
|Author||Dr Maria Chernyakova|
|Description||Gamma-ray-loud binary systems (GRLB) are X-ray binaries which emit VHE gamma rays . Only 4 such systems, have been detected as persistent or regularly variable TeV emitters. The source of the high-energy activity of these GRLBs is uncertain. For understanding the nature of GRLBs a larger number of similar objects is required. Most of the variable and transient Galactic sources of GeV gamma-rays are expected to belong to the GRLB class. We produced a variability map of GC plane at 300MeV -- 300GeV using more than 3years of FERMI data, that allowed to identify 3 variable unidentified sources, that are candidates to GRLBs. We propose the 10ksec XMM observation of each of these sources to determine the nature of these sources and to check whether these sources are GRLBs.|
|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, 2013-10-09T00:00:00Z, 069198, 17.56_20190403_1200. https://doi.org/10.5270/esa-79nr2qd|