Examining Dust Grain Models Using the Reddening and X-Ray Dust Halo of Terzan 2

Details Examining Dust Grain Models Using the Reddening and X-Ray Dust Halo of Terzan 2 Examining Dust Grain Models Using the Reddening and X-Ray Dust Halo of Terzan 2

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...692..502v&link_type=abstract

The Astrophysical Journal, Volume 692, Issue 1, pp. 502-510 (2009).

Astronomy and Astrophysics

Astronomy

3

Dust, Extinction, Globular Clusters: Individual: Terzan 2, X-Rays: Ism

Scientific paper

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 interstellar medium along this line of sight (LOS). The X-ray dust halo arises from X-rays scattering off of interstellar dust grains. Using a low optical depth sight line to determine the Chandra ACIS point-spread function, we extracted the radial profile as a function of energy and used it to determine the H column density (N H) and cloud location along the LOS for several dust grain models, including the commonly-used models of MRN and WD. The resulting N H values were used to determine the reddening E(B - V), which was then compared with the average E(B - V) for this sight line found by other workers. We found that for this LOS, only the ZDA BARE-AC-S, BARE-GR-FG, and BARE-GR-S models yield reddenings within 1σ of the literature average.

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