A Fourier Transform Telescope for Sub-arcsecond Imaging of X-Rays and Gamma Rays
This paper describes a Fourier transform telescope designed to image solar flare X-rays and gamma rays at energies up to 1 MeV with arcsecond or subarcsecond resolution. The imaging technique makes use of a bigrid collimator divided into a number of smaller areas called subcollimators. The grids in each subcollimator consist of a set of linear apertures so configured that each subcollimator provides a measurement of a single Fourier component of the angular distribution of the source. The imaging concept is therefore a mathematical analog to aperture synthesis in radio astronomy. For X-ray and gamma-ray astronomy, this approach has significant advantages in terms of relaxed requirements for position sensitivity in the detector and for control of grid alignment in the large scale telescope structure. The concept of the Fourier transform telescope will be illustrated with numerical parameters of a version now under study for the Pinhole/Occulter Facility.
Additional Information© 1985 SPIE. The imaging techniques described here have been stimulated by contributions form a large number of individuals throughout the high-energy solar physics and astrophysics community. Extensive discussion and review has come from NASA working groups and study teams, namely the Hard X-ray Imaging Facility Definition Team under L. E. Peterson, the Pinhole/Occulter Facility Science Working Group under H. R. Hudson and E. Tandberg-Hanssen, The MAX '91 Science Study Committee under B. R. Dennis, and the High-Energy Facility Workshop for the Advanced Solar Observatory under E. P. Chupp. At Caltech this work is supported by NSF grant ATM-83-09955 and NASA grant NGR 05-002-160.
Submitted - 1985-25.pdf