|Title||The 44 ms Pulsar Powering HESS J1813-178|
|Author||Dr Eric Gotthelf|
|Description||We have just discovered the pulsar in the faint shell-type supernova remnant SNR G12.82-0.02, coincident with the TeV source HESS J1813-178 and possibly the Fermi source 0FGL J1814.3-1739. PSR J1813-1749 is clearly one of the most energetic pulsars in the Galaxy, but its spin-down power is poorly measured. We need a brief follow-up observation to measure the all-important period derivative, critical to determining the energetics, dipole magnetic field strength, and spin-down age. This will allow us to infer the efficiency of emission in all high-energy wavebands from X-ray through TeV, and to search for GeV pulsations with Fermi. We can also constrain the age of the SNR and the birth period of the pulsar, important for modeling the radiation and evolution of the system.|
|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, 2012-04-01T00:00:00Z, 065031, 17.56_20190403_1200. https://doi.org/10.5270/esa-gha8is1|