HRMA calibration handbook: EKC gravity compensated XRCF models

Details HRMA calibration handbook: EKC gravity compensated XRCF models HRMA calibration handbook: EKC gravity compensated XRCF models

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994axaf.reptq....t&link_type=abstract

Performance Report Smithsonian Astrophysical Observatory, Cambridge, MA. Advanced X-Ray Astrophysics Facility.

Astronomy and Astrophysics

Astrophysics

Calibrating, Computerized Simulation, Handbooks, Mirrors, Ray Tracing, X Ray Astrophysics Facility, Computer Programs, Finite Element Method, Spacecraft Structures, Telescopes

Scientific paper

This document, consisting of hardcopy printout of explanatory text, figures, and tables, represents one incarnation of the AXAF high resolution mirror assembly (HRMA) Calibration Handbook. However, as we have envisioned it, the handbook also consists of electronic versions of this hardcopy printout (in the form of postscript files), the individual scripts which produced the various figures and the associated input data, the model raytrace files, and all scripts, parameter files, and input data necessary to generate the raytraces. These data are all available electronically as either ASCII or FITS files. The handbook is intended to be a living document and will be updated as new information and/or fabrication data on the HRMA are obtained, or when the need for additional results are indicated. The SAO Mission Support Team (MST) is developing a high fidelity HRMA model, consisting of analytical and numerical calculations, computer software, and databases of fundamental physical constants, laboratory measurements, configuration data, finite element models, AXAF assembly data, and so on. This model serves as the basis for the simulations presented in the handbook. The 'core' of the model is the raytrace package OSAC, which we have substantially modified and now refer to as SAOsac. One major structural modification to the software has been to utilize the UNIX binary pipe data transport mechanism for passing rays between program modules. This change has made it possible to simulate rays which are distributed randomly over the entrance aperture of the telescope. It has also resulted in a highly efficient system for tracing large numbers of rays. In one application to date (the analysis of VETA-I ring focus data) we have employed 2 x 107 rays, a substantial improvement over the limit of 1 x 104 rays in the original OSAC module. A second major modification is the manner in which SAOsac incorporates low spatial frequency surface errors into the geometric raytrace. The original OSAC included the ability to use Legendre-Fourier polynomials to describe deviations from the basic optical prescription. To this we have added bicubic splines to address a deficiency in the handling of the sharper deformations in the areas of mirror support pads. SAO has developed software (TRANS-FIT) to translate the most common finite element analysis models into these forms for incorporation into the raytrace program.

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