Solar Physics Division Meeting 2000, June 19-22
Session 2. Corona, Solar Wind, Flares, CMEs, Solar-stellar, Instrumentation, Other
Display, Chair: J. Krall, Monday-Thursday, June 19, 2000, 8:00am-6:00pm, Forum Ballroom

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[2.95] The Imaging Capabilities of HESSI

E.J. Schmahl (UMd & NASA/GSFC), HESSI Team

The High Energy Solar Spectroscopic Imager (HESSI) will use rotational modulation synthesis for mapping hard X-ray and gamma-ray flares with spatial resolution of 2.3'' and spectral resolution of ~ 1 keV. Like the Yohkoh/HXT hard X-ray telescope, HESSI relies on Fourier methods to produce images, but HESSI has many more sampled points in the Fourier plane, and is expected to produce higher resolution maps with greater dynamic range.

We summarize the methods to be used for HESSI imaging, touching on crucial details of modulation such as the Calibrated Event List, and describing the Back Projection method. Beyond these, we outline four basic tools for image reconstruction: CLEAN, MEM, PIXONS, and Forward Fitting. We present examples of simulated images for the existing reconstruction tools, with estimates of photometry and required computer resources.

Support for this work was provided by grant NAG-58849 from Goddard Spaceflight Center to the University of Maryland.

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