|Title||Unveiling the timing behaviour of the radio-quiet Vela-like pulsar J1826-1256|
|Author||Dr Massimiliano Razzano|
|Description||The radio-quiet gamma-ray pulsars discovered by Fermi Large Area Telescope are crucial to understand pulsar magnetospheres and the Galactic neutron star population. We propose a deep XMM observation of PSR J1826-1256, the young, energetic radio-quiet pulsar in the "Eel" nebula. Its timing parameters and gamma-ray properties are similar to those of the Vela pulsar. Comparing its X and gamma-ray emission with other Vela-like, but radio-loud, pulsars will help to probe the nature of radio quietness-loudness in pulsars. We will exploit XMM to search for X-ray pulsations of the X-ray bright PSR J1826-1256, detail its timing and spectral behaviour, and discriminate the pulsar emission from that of its nebula by using archival Chandra data.|
|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, 2015-11-04T23:00:00Z, 074442, 17.56_20190403_1200. https://doi.org/10.5270/esa-2gs92wi|