|Title||The Rapidly Variable Iron K Line in Mkn 279|
|Author||Dr Kimberly Weaver|
|Description||We request a 30 ks XMM observation of Mkn 279, an X-ray bright Seyfert 1 galaxy with a time-variable iron K-alpha line, to study changes in the accretion disk. During a virgul1-day ASCA observation ,the iron line energy increased from 6.4 keV to 6.6 keV in the rest frame as the source flux increased by 20 percent. This rapid response of the iron line to the continuum implies that we are watching changes occur in the inner regions of the accretion disk near the black hole. Such changes may take the form of an ionization increase, enhanced Doppler effects, or changes in the illumination of the disk. The iron line profile in Mkn 279 is relatively simple compared to the well-known but enigmatic emission line in MCG-6-30-15, and so it will be much easier to study.|
|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, 2003-06-06T00:00:00Z, 008396, 17.56_20190403_1200. https://doi.org/10.5270/esa-tm9qjs5|