|Title||MRK 421: COORDINATED MULTI-MISSION HIGH-ENERGY STUDY OF A REMARKABLE BLAZAR|
|Author||Dr Daniela Dorner|
|Description||The goal is to understand the low-flux state and long-term behaviour of blazars at high-energies by studying Mrk 421 with a combination of observations from X-rays to TeV gamma rays, with two INTEGRAL observations of 370 ks each, one in each of the visibility periods in Maya??June and Nova??Dec. These observations will be enhanced with snapshots with XMM-Newton and Swift, and public monitoring programs by Fermi and Swift-XRT. The energy ranges covered by INTEGRAL and FACT are crucial for modelling the SED of blazars; we want to investigate the behaviour on timescales of months, to constrain blazar emission models. Comparing two observations, we want to investigate if Mrk 421 exhibits a peak shift and thus a tendency to extreme behaviour (as Mrk 501 and 1ES 2344+51.4).|
|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, 2022-01-31T00:00:00Z, 085360, 19.17_20220121_1250. https://doi.org/esa-[xxxxxxx]|