|Title||Resolving the mystery of FRI particle content|
|Author||Dr Judith Croston|
|Description||Understanding the dynamics and energetics of low-power (FR I) radio galaxies is essential to constrain their feedback role in galaxy groups and clusters, but it has long been known that their relativistic electron population and magnetic fields cannot provide enough pressure to balance the measured external pressure if at equipartition. Our recent XMM-Newton studies of FR I radio-galaxy environments reveal the first direct evidence that entrainment of material from the hot-gas environment provides the necessary particle population: the apparent pressure imbalance is linked to radio morphology. We propose to observe a small sample of bridged-morphology FRIs to test the prediction that their lobes should be close to pressure balance at equipartition.|
|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, 2009-09-26T00:00:00Z, 055027, 17.56_20190403_1200. https://doi.org/10.5270/esa-2tcmyo2|