|Title||The 8 keV line in the X-ray bright Seyfert galaxy UGC 3973|
|Author||Dr Luigi Gallo|
|Description||Two short exposures of the bright, radio-quiet Seyfert1.2 galaxy UGC3973 were conducted with XMM as part of an AGN snap-shot survey. During one of these observations a narrow 8keV (rest frame) line-like emission feature was detected with the pn instrument. An instrumental origin was ruled out. The detection was seriously scrutinised and found to be significant at 96.0-98.4% confidence, depending what a priori assumptions were made. We propose three, 20ks observations (60ks total) of UGC3973 spread over AO5. The proposed programme will allow investigation of the significance of the feature, its variability, and its origin. In addition, UGC3973 has demonstrated significant flux and spectral variability over similar time periods as proposed here. This will allow|
|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, 2008-04-20T00:00:00Z, 040007, 17.56_20190403_1200. https://doi.org/10.5270/esa-9himi2w|