|Title||Do GRBs occur in galaxies with AGN?|
|Author||Dr Myrto Symeonidis|
|Description||Currently, long duration GRBs (LGRBs) are thought to be triggered by the collapse of a massive low metallicity star, establishing them as powerful probes of massive star-formation in young galaxies out to the early epochs of galaxy formation. However, to date, the properties of their host galaxies at high redshift are not well understood. In particular, although we know of LGRB host galaxies in the ULIRG regime, we do not yet know whether LGRB hosts are ever home to AGN and whether the AGN, if present, has evolved sufficiently to be an active participant in the evolution of the system. Determining the stage of black hole growth in LGRB hosts would thus bring us closer to understanding the stages of galaxy evolution for which the star formation history can be probed using GRBs.|
|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, 2015-01-20T23:00:00Z, 072415, 17.56_20190403_1200. https://doi.org/10.5270/esa-5z64qdi|