|Title||Iron line Doppler tomography with quasi-periodic oscillations|
|Author||Dr Adam Ingram|
|Description||We propose three joint XMM-Newton and NuSTAR observations of the black hole binary H 1743-322, each covering a single XMM-Newton orbit and 70ks of NuSTAR time, sampling different stages of spectral evolution during the rise to outburst. This builds upon our recent discovery that the iron line centroid energy in this source varies systematically over the course of a 4s QPO cycle, providing strong evidence that the QPO is driven by relativistic precession. We now aim to sample the same source when displaying a range of higher QPO frequencies to explore the evolution of the iron line profile phase dependence with QPO frequency and compare with the prediction of relativistic precession. We will trigger the observations from Swift monitoring throughout the outburst.|
|Publication||No observations found associated with the current proposal|
|Instrument||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, 2019-10-22T22:00:00Z, 078354, 19.17_20220121_1250. https://doi.org/10.5270/esa-pmib357|