|Title||OM Photometric Calibration using Abell 3195|
|Author||Mr Fred Jansen XMM-Newton PS|
|Description||CAL-The primary goal of the observation Abell 3195 is to establish the zero point calibration of the OM V filter. The photometric calibration of the magnifier (and of the B filter) are another goal of that observation. Secondary calibration item is the measurement of the instrument PSF, which is accomplished by placing fast mode windows on two field stars. The change of count rate and PSF with window size is the purpose of introducing exposures with small image mode windows in the V-filter and the magnifier. The estimated OM overhead time is 3.8 ksec.|
|Publication||The XMM-Newton serendipitous ultraviolet source survey catalogue . Page, M. J., Brindle, C., et all. . MNRAS . 426-903 . 2012 . 2012MNRAS.426..903P ,
|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, 2000-03-09T00:00:00Z, 009964, 17.56_20190403_1200. https://doi.org/10.5270/esa-padlfjt|