The Calibration of the Solar-B X-ray Telescope (XRT)

Details The Calibration of the Solar-B X-ray Telescope (XRT) The Calibration of the Solar-B X-ray Telescope (XRT)

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp43a..01g&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP43A-01

Computer Science

Performance

2794 Instruments And Techniques, 7513 Coronal Mass Ejections, 7549 Ultraviolet Emissions, 7554 X Rays, Gamma Rays, And Neutrinos, 7594 Instruments And Techniques

Scientific paper

The Solar-B X-ray telescope (XRT) is designed to have a wide temperature sensitivity in order to observe and analyze both the high (5-10 MK) and low temperature (1-5 MK) phenomena in the coronal plasma. It will be the telescope with the highest resolution ever flown for solar coronal studies. The telescope is designed for full Sun imaging over the wavelength range 6-60 Angstroms. The XRT is a grazing-incidence modified Wolter I X-ray telescope, of 35 cm inner diameter and 2.7 m focal length. The 2048 X 2048 back illuminated CCD has 13.5 µm pixels, corresponding to 1 arcsecond. The filter set used in the XRT, mounted at the telescope entrance and near the focal plane, will perform three functions: (1) to reduce the heat load inside the telescope, (2) to reduce the incoming visible light and (3) to provide spectral diagnostics to determine coronal plasma temperatures. This paper will present the results of the XRT calibration performed at the X-ray Calibration Facility, NASA-MSFC, Huntsville, Alabama in January 2005. We will discuss the methods and the most significant results of the XRT performance, namely: imaging properties, encircled energy, the point response function and the effective area in the 0.2-2 keV energy range.

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