|Title||Line Dominated Quiescent X-ray Emission from the X-ray transient XTE J0421+560|
|Author||Dr Arvind Parmar|
|Description||In AO1 we were awarded a 30 ks Priority A observation of the soft X-ray transient XTE J0421+560 in quiscence. Due to intervals of high particle background only 12 ks of good observing time was obtained. However, even with this limited exposure it is clear that the observed spectrum is unlike anything ever seen in the X-ray sky before. The spectrum is totally dominated by a broad emission feature at 6.9 keV which may have a narrow core. There may be a second broad Gaussian feature at 1.0 keV. There is no X-ray continuum present with an upper limit of <3% of the line flux. We propose a 60 ks XMM-Newton observation of XTE J0421+560 in order to provide a high quality spectrum which will allow us to study this unique object in detail.|
|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, 2004-03-14T00:00:00Z, 013976, 17.56_20190403_1200. https://doi.org/10.5270/esa-gjhcaf5|