Volume 496, Number 3, March IV 2009
|Page(s)||879 - 889|
|Published online||30 January 2009|
Statistical evaluation of the flux cross-calibration of the XMM-Newton EPIC cameras
Department of Physics and Astronomy, University of Leicester, University Road, Leicester, UK e-mail: firstname.lastname@example.org
2 XMM SOC, ESAC, Apartado 78, 28691 Villanueva de la Cañada, Madrid, Spain
Accepted: 20 January 2009
Context. The second XMM-Newton serendipitous source catalogue, 2XMM, provides the ideal data base for performing a statistical evaluation of the flux cross-calibration of the XMM-Newton European Photon Imaging Cameras (EPIC).
Aims. We aim to evaluate the status of the relative flux calibration of the EPIC cameras on board the XMM-Newton observatory (MOS1, MOS2, and pn) and investigate the dependence of the calibration on energy (from 0.2 to 12.0 keV), position of the sources in the field of view of the X-ray detectors, and lifetime of the mission.
Methods. We compiled the distribution of flux percentage differences for large samples of “good quality” objects detected with at least two of the EPIC cameras. The mean offset of the fluxes and dispersion of the distributions was then found by Gaussian fitting. Count rate to flux conversion was performed with a fixed spectral model. The impact on the results of varying this model was investigated.
Results. Excellent agreement was found between the two EPIC MOS cameras to better than 4% over the entire energy range where the EPIC cameras are best calibrated (0.2-12.0 keV). We found that MOS cameras register 7-9% higher flux than EPIC pn below 4.5 keV and a 10-13% flux excess at the highest energies (4.5 keV). No evolution of the flux ratios is seen with time, except at the lowest energies (0.5 keV), where we found a strong decrease in the MOS to pn flux ratio with time. This effect is known to be due to a gradually degrading MOS redistribution function. The flux ratios show some dependence on distance from the optical axis in the sense that the MOS to pn flux excess increases with off-axis angle. Furthermore, in the 4.5-12.0 keV band there is a strong dependence of the MOS to pn excess flux on the azimuthal-angle. These results strongly suggest that the calibration of the Reflection Grating Array (RGA) blocking factors is incorrect at high energies. Finally, we recommend ways to improve the calculation of fluxes in future versions of XMM-Newton serendipitous source catalogues.
Key words: instrumentation: detectors / methods: statistical / space vehicles: instruments / X-rays: general
© ESO, 2009
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