CAL-The primary goal of the observation of the white dwarf BPM 16274 is toestablish the zero point calibration of the OM UV filter. Secondary calibrationitem is the measurement of the instrument PSF in the UV filters, which isaccomplished by placing a fast mode window at the location of BPM 16274. Thetarget count rate and the PSF shape is studied under count to framerate ratiosby changing the window size. The study also includes an OM defaultconfiguration. The modification of the PSF with window size is best studied withthe magnifier. The UV grism wavelength and PSF shape can be calibrated makinguse of the available spectrum. The estimated OM overhead time is 8.1 ksec forthe initial and 4.3 ksec for the follow up observations.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2000-05-18T06:49:45Z/2000-05-18T22:47:29Z
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, Mr Fred Jansen XMM-Newton PS, 2001, 'OM UV Photometric Calibration using BPM 16274', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-iwjaupx
