Optimizing RHESSI X-ray Imaging

Details Optimizing RHESSI X-ray Imaging Optimizing RHESSI X-ray Imaging

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9306d&link_type=abstract

American Astronomical Society Meeting 210, #93.06; Bulletin of the American Astronomical Society, Vol. 39, p.212

Astronomy and Astrophysics

Astronomy

Scientific paper

RHESSI X-ray imaging is possible with angular resolution as fine as 2 arcsec (FWHM) at energies from as low as 3 keV to >100 keV. However, taking full advantage of this capability has proven to be challenging given the Fourier-transform imaging technique that is used, specific instrumental considerations that must be taken into account, and the many different options of the available image reconstruction algorithms. Such considerations as the best reconstruction algorithm to use, the optimal weighting of the different Fourier components, deciding between short image integration times and rapid imaging cadence, the different energy ranges covered by the 9 detectors, the effect of pulse pile-up and albedo, etc. must all be taken into account in obtaining and interpreting RHESSI X-ray images. This poster describes different techniques for optimizing the image reconstruction depending on the science objectives - identifying compact or extended sources, searching for source motion, obtaining the best photometry, determining the believability of different features in an image, etc. The emphasis is on making full use of data from all the RHESSI detectors, including the ones behind the finest grids when warranted by the source structure. This is the case for the hard X-ray emission along the ribbons of the flare on 2005 May 13 reported by Liu et al. (2007) and this event will be used as an example.
Liu, C. and Lee, J. and Gary, D. E. and Wang, H., “The Ribbon-like Hard X-Ray Emission in a Sigmoidal Solar Active Region", ApJ., 658, L127-L130, 2007.

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