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CONTENTS: Optics Description | Calibration

Optics Description

The XRT Mirror Assembly consists of the X-Ray Mirror Module, a thermal baffle, a mirror collar and an electron deflector. The mirror set used by XTR was built and calibrated for the JET-X program. The mirror module (see picture on the left) has 12 concentric gold-coated electroformed Ni shells with focal lenght of 3500mm. In order to optimize the angular resolution over the field of view the detector is slightly defocused. Temperature gradients in the mirror can affect and distort the figure and the Point Spread Function. To avoid this problem a thermal baffle controlled by heaters balance the heat lost to space by the mirrors. An electron deflector, consisting of a system of 12 rare earth magnets, installed on the OBIF behind the rear face of the mirror module prevents electrons that pass through th mirror from reaching the detector.


CONTENTS: Optics Description | Calibration


The XRT mirros were calibrated at Panter in 1996 for the JET-X calibration plan and again in 2000 during the XRT end-to-end calibration. Five different energies were used in the four XRT operational modes, both on and off-axis.

Energy (KeV)

Calibration images (for two sources displaced by 20arcsec) and the measured angular resolution of the mirrors are shown in the figure.

Calibration of the PSF and the effective area have been performed at Panter X-ray calibration facility. The calibration source was positioned at 130meters from the mirros. Corrections for the divergence of the X-ray beam and for pile-up effects have been applied. In the figures below the results of the effective area calibration tests in Window Timing and Photo-Diode modes are shown. The data for the PSF calbiration have been taken in imaging mode with more than 1000 counts in the image with a countrate lower than 10000counts/s. The PSF profile has fitted by a model composed by a Gaussian function for the central part of the profile and a King function for the PSF wings. An examples of PSF profile is shown in this figure. The PSF is slightly blurred on axis and better at 7arcmin off-axis due to the fact that the CCD is intentionally offset along the optical axis from the best on-axis focus. An analytical model to describe the PSF as a function of energy and angle was contructed to calculate the PSF correction for a source with a generic spectrum in a generic position of the detector. This model always described the data with a precision better than 2%. The mission requirements for the effective area, the PSF and the spatial resolution were met at the Panter Facility and through the detailed study of the PSF and the analytical model the PSF correction for astronomical sources can be calculated with great accuracy.

Mullard Space Science Laboratory Southwest Research Institute Osservatorio Astronomico di Brera Penn State University University of Leicester Goddard Space Flight Center Max Planck Institute Agenzia Spaziale Italiana Sonoma State University Omitron Institution Menu