An Analysis of the X-ray Dust Halo Toward 4U 1724-307

Details An Analysis of the X-ray Dust Halo Toward 4U 1724-307 An Analysis of the X-ray Dust Halo Toward 4U 1724-307

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.1408v&link_type=abstract

American Astronomical Society, AAS Meeting #212, #14.08; Bulletin of the American Astronomical Society, Vol. 40, p.530

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We use the X-ray dust halo of the low mass X-ray binary 4U 1724-307, located in the globular cluster Terzan 2, to probe the ISM along this line of sight. The X-ray dust halo arises from scattering off interstellar dust grains. Using a low optical depth sightline to determine the Chandra ACIS point-spread function, we extracted the radial prole as a function of energy and used it to determine the H column density (NH) and cloud location along the line of sight for 17 dust grain models, including the commonly-used models of MRN and WD. The resulting NH values were used to determine the reddening E(B-V), which was then compared to the average E(B-V) for this sight line found by other workers. Our results indicate that most models we tested cannot yield reddenings in agreement with the literature average.

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