|Title||Pulse-phase spectroscopy of the anomalous X-ray pulsar 1E 1048.1-5937 in a low|
|Author||Dr Andrea Tiengo|
|Description||1E 1048.1-5937 is the magnetar candidate with the largest pulsed fraction, that is observed to be anti-correlated to the source flux. At the lowest flux level, the 1-10 keV pulsed fraction is >90% and a soft X-ray spectral component, possibly due to thermal emission from most of the magnetar surface, emerges at pulse-phase minimum. This source state provides the best opportunity to study through phase-resolved spectroscopy both the non-thermal and thermal emission from regions of the magnetar surface at different temperatures. Since the only available observation of 1E 1048.1-5937 in this low flux state is a 5 ks XMM-Newton observation, we propose a deeper 80 ks observation, to be performed in case the 2-10 keV flux falls below 4E-12 erg cm-2 s-1.|
|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, 2012-09-10T00:00:00Z, 065487, 17.56_20190403_1200. https://doi.org/10.5270/esa-3slcx5g|