|Title||Search for crushed plerions: TeV to X-ray connection|
|Author||Dr Oleg Kargaltsev|
|Description||We propose a mini-survey of unidentified TeV sources having young Vela-like pulsars with known X-ray PWNe as their neighbors. Although these pulsars show 10.-15. offsets from the center of the TeV brightness distribution, they are likely to be connected to the nearby TeV sources through a faint asymmetric X-ray nebulae formed as a result of the interaction between the SNR reverse shock and the pulsar wind. To test this, we propose to obtain deep X-ray images of several crushed PWN candidates to search for correlations between the X-ray and TeV emission. Confirming that the X-ray PWNe are preferentially extended toward the neighboring TeV sources will establish the viability of the crushed PWN model and reveal the nature of the currently unidentified TeV sources.|
|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, 2008-11-14T00:00:00Z, 050317, 17.56_20190403_1200. https://doi.org/10.5270/esa-jift5fn|