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The Swift X-ray Telescope focal plane camera is a front-illuminated MOS CCD,providing a spectral response kernel of 135 eV FWHM at 5.9 keV as measuredbefore launch. We describe the CCD calibration program based on celestial andon-board calibration sources, relevant in-flight experiences, and developmentsin the CCD response model. We illustrate how the revised response modeldescribes the calibration sources well. Comparison of observed spectra withmodels folded through the instrument response produces negative residualsaround and below the Oxygen edge. We discuss several possible causes for suchresiduals. Traps created by proton damage on the CCD increase the chargetransfer inefficiency (CTI) over time. We describe the evolution of the CTIsince the launch and its effect on the CCD spectral resolution and the gain.

The in-flight spectroscopic performance of the Swift XRT CCD camera during 2006-2007