CAL- The bright LMC X-3 binary will be observed with the EPIC cameras to tracethe PSF out into the wings. By use of different modes some correction forpile-up may be achieved. The target ideally should be measured in its lowestflux state to minimise pile-up effects. The Full window modes will capturethe 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. Asmall window mode in each case will be used measure the PSF core. (Assumed 2x2.7ksec overhead for EPIC in defining RGS and OM exposures). Tho observation maybe repeated at a lower flux state of the source, by rescheduling ca. 45 daysafter the first observation.
Instrument
EMOS1, EMOS2, EPN, RGS1, RGS2
Temporal Coverage
2000-06-09T06:54:19Z/2000-06-10T07:00:09Z
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 Fred Jansen XMM-Newton PS, 2001, 'LMC X-3 High S:N Point Spread Functions in EPIC', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-nz4itfl
