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Our goal is to validate the CXC's telescope model to ensure that the
on-orbit PRF can be reliably modeled at any axial location and for
arbitrary source spectral energy distribution. Our analysis strategy
is shown schematically in Figure 1. The
parameters for each test, defined by its TRW identification code, are
taken from the so-called as run Calibration Measurement Data Base
(CMDB). The parameters for each test drawn from the CMDB (e.g. ACIS
mode, axial location, defocus position, etc.) served as boundary
conditions to SAOSAC+MARX models. The SAOSAC raytrace included
corrections for gravity ovalization, finite source distance geometry,
mirror misalignments, and the ~10% reduction in effective area
discovered during Phase F. The ACIS model is a simple
``slab-and-stop'' detector model capable of treating charge spreading
between pixels, but does not include a detailed treatment of the
sub-pixel structure on the front illuminated (FI) devices, nor does it
include a back illuminated (BI) model device. The ``Analysis'' box
lists the analysis methods applied identically to both XRCF and model
images and spectra (we discuss each in detail below). When the data
and model analyses disagreed, certain model parameters were adjusted
in an attempt to attain agreement between the model and data. The
model can be applied to on-orbit imaging by removing the compensation
for ground effects from the model. We intend to repeat this
validation procedure using on-orbit data.
Figure 1:
Schematic of data analysis strategy.
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Next: ACIS Data Acquisition Modes
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Alexandria Ware
1999-03-29