After 3 years of all-sky scanning, Fermi has discovered dozens of new g-ray onlypulsars. Such a discovery has far reaching implications for our overallunderstanding of pulsar physics. We propose a joint XMM-Chandra observation ofJ1813-1246, one of the most energetic g-ray selected pulsar. J1813 rotates asfast as the Crab and its Erot is similar to that of Vela, thus we expect thepulsar to be embedded in a bright PWN. Among RQ pulsars, J1813 shows the highestX-ray flux but no deep X-ray observations have ever been performed on thistarget. Exploiting both XMM and Chandra capabilities we ll be able to (i)discriminate J1813 from its pulsar wind nebula (ii) study its X-ray timingbehaviour (iii) obtain accurate phase-averaged and phase-resolved spectra (iv) constrain the source distance.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2013-03-10T08:37:15Z/2013-03-11T14:52:34Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Dr Martino Marelli, 2014, 'Unveiling the pulsating behaviour of J1813 comma a very energetic radio-quiet pulsar', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-bh24i9k
