Using the Chandra Source-Finding Algorithm to Automatically Identify Solar X-ray Bright Points

Details Using the Chandra Source-Finding Algorithm to Automatically Identify Solar X-ray Bright Points Using the Chandra Source-Finding Algorithm to Automatically Identify Solar X-ray Bright Points

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1519a&link_type=abstract

American Astronomical Society, SPD meeting #40, #15.19; Bulletin of the American Astronomical Society, Vol. 41, p.838

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Scientific paper

This poster details a technique of bright point identification that is used to find sources in Chandra X-ray data. The algorithm, part of a program called LEXTRCT, searches for regions of a given size that are above a minimum signal to noise ratio. The algorithm allows selected pixels to be excluded from the source-finding, thus allowing exclusion of saturated pixels (from flares and/or active regions). For Chandra data the noise is determined by photon counting statistics, whereas solar telescopes typically integrate a flux. Thus the calculated signal-to-noise ratio is incorrect, but we find we can scale the number to get reasonable results. For example, Nakakubo and Hara (1998) find 297 bright points in a September 11, 1996 Yohkoh image; with judicious selection of signal-to-noise ratio, our algorithm finds 300 sources. To further assess the efficacy of the algorithm, we analyze a SOHO/EIT image (195 Angstroms) and compare results with those published in the literature (McIntosh and Gurman, 2005). Finally, we analyze three sets of data from Hinode, representing different parts of the decline to minimum of the solar cycle.

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