Physics – Optics
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.4610g&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #46.10; Bulletin of the American Astronomical Society, Vol. 24, p.1196
Physics
Optics
Scientific paper
We present the results of applying image reconstruction and deconvolution techniques to simulated astrod X-ray images. We use the Richardson--Lucy and Maximum Entropy methods to assess the potential for reconstructing images of astronomical sources. X-ray sky fields are modeled using calibration and ray--tracing results and include the effects of the X-ray and particle background. We characterize the ability of the above methods to resolve sources for a range of off-axis pointings, f1ux and background levels, and spectral compositions. The astrod mission, to be launched in February 1993, will provide broad-band (1-10 keV) X-ray imaging with a large effective area (1300 cm(2) at 1 keV and 600 cm(2) at 7 keV). The satellite includes four independent grazing incidence X-ray telescopes with two CCD detectors (~2 arcsec position resolution) and two position sensitive Xenon scintillation counters ( ~ 0.5 arcmin position resolution) at their respective focal planes. The optics were developed at NASA Goddard Space Flight Center and comprise a nest of 120 thin--foil mirror pairs, which have a conical profile rather than the parabola-hyperbola combination of the Wolter I design. The mirror design results in a complex Point Spread Function (PSF) with a strong azimuthal dependence which varies as a function of off--axis position. The radial profile has a sharp core and weak extended wings making it similar in shape to the Hubble Space Telescope PSF caused by the spherical aberration. The Half Energy Width (HEW) of the astrod PSF is ~ 3 arcmin. Image reconstruction and deconvolution techniques, such as those used for the Hubble telescope, will play an important role for astrod imaging. For data of sufficiently high signal to noise ratio, the sharp core of the foil mirrors should resolve point sources separated by only 20 arcsecs and allow higher resolution images to be obtained.
Gotthelf Eric Van
Jalota Lalit
Zoonematkermani Saeid
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