|LMC X-3 High S:N Point Spread Functions in EPIC
|Dr Fred Jansen XMM-Newton PS
|CAL- The bright LMC X-3 binary will be observed with the EPIC cameras to trace the PSF out into the wings. By use of different modes some correction for pile-up may be achieved. The target ideally should be measured in its lowest flux state to minimise pile-up effects. The Full window modes will capture the wings of the PSF to high S:N with minimnal confusion from background and serendipitous sources, but significant pile-up will occur in the PSF core. A small window mode in each case will be used measure the PSF core. (Assumed 2x 2.7ksec overhead for EPIC in defining RGS and OM exposures). Tho observation may be repeated at a lower flux state of the source, by rescheduling ca. 45 days after the first observation.
|No observations found associated with the current proposal
|EMOS1, EMOS2, EPN, OM, RGS1, RGS2
|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
|European Space Agency, 2000, 012331, 17.56_20190403_1200. https://doi.org/10.5270/esa-ae0c4jq