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We desire a simple comparison of the absolute effective areas of the currentgeneration of CCD instruments onboard the following observatories: ChandraACIS-S3, XMM-Newton (EPIC-MOS and EPIC-pn), Suzaku XIS, and Swift XRT and astraightforward comparison of the time-dependent response of these instrumentsacross their respective mission lifetimes. We have been using 1E 0102.2-7219,the brightest supernova remnant in the Small Magellanic Cloud, to evaluate andmodify the response models of these instruments. 1E 0102.2-7219 has stronglines of O, Ne, and Mg below 1.5 keV and little or no Fe emission to complicatethe spectrum. As part of the activities of the International AstronomicalConsortium for High Energy Calibration (IACHEC), we have developed a standardspectral model for 1E 0102.2-7219. The model is empirical in that it includesGaussians for the identified lines, an absorption component in the Galaxy,another absorption component in the SMC, and two thermal continuum components.In our fits, the model is highly constrained in that only the normalizations ofthe four brightest lines/line complexes (the O vii He$\alpha$ triplet, O viiiLy$\alpha$ line, the Ne ix He$\alpha$ triplet, and the Ne x Ly$\alpha$ line)and an overall normalization are allowed to vary. We have examined thesemeasured line fluxes as a function of time for each instrument after applyingthe most recent calibrations that account for the time-dependent response ofeach instrument. We perform our effective area comparison with representative,early mission data when the radiation damage and contamination layers were at aminimum. We find that the measured fluxes of these lines generally agree towithin +/-10% for all instruments, with 38 of our 48 fitted normalizationswithin +/-10% of the IACHEC model value.

astronomy and astrophysics

SNR 1E 0102.2-7219 as an X-ray Calibration Standard in the 0.5-1.0 keV  Bandpass and Its Application to the CCD Instruments aboard Chandra, Suzaku,  Swift and XMM-Newton