|Title||Multiwavelength spectral variability of Very-High-Energy Blazar Outbursts|
|Author||Ms Andrea Gokus|
|Description||We propose a 100 ks ToO observation of a blazar in outburst as detected by the FACT TeV gamma-ray telescope, supplemented by pre-outburst snapshots and follow- up monitoring with Swift. Bright TeV gamma-ray flares have been detected frequently from blazars, but complete information of the multiwavelength spectra before, during and after an outburst are not available. Leptonic models for TeV flares predict simultaneous flux increases in the X-ray and in the gamma-ray band. Other types of TeV flares, which cannot be explained with current models, are also observed, such as orphan flares, which show little to no variability in the X-rays. XMM-Newton will add high-sensitivity spectra to our already set-up FACT and INTEGRAL ToO program.|
|Publication||No observations found associated with the current proposal|
|Instrument||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, 2020-07-11T22:00:00Z, 084500, 19.17_20220121_1250. https://doi.org/10.5270/esa-gssxqjh|