DIRTY Spherical Galacitic Environment Data

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These model runs use the Weingartner & Draine 2001, ApJ, 548, 296 dust grain models for MW, LMC2, and SMC dust. The dust grain model scattering parameters were downloaded from Bruce Draine's homepage. They also cover a wider range of wavelengths (0.05 - 3 microns) than the Witt & Gordon (2000) models which used empirically determined dust scattering properties. The inputs are significantly different than those used in the original tables and are probably not as valid as those used in that paper. Dust grain models do not use the known dust scattering properties as constraints and, thus, do not do a good job reproducing them. It is not clear which dust grain model inputs should be used, especially in the case of SMC or LMC type dust or at wavelengths where the empirical work has not been done. For the MW runs, the empirical dust grain inputs (original calculations) are the recommened inputs. More work is obviously needed on both empirically determining dust grain scattering inputs in other galaxies as well as inproving the dust grain models to include the empirical work on dust scattering properties.

geometry, dust-typek2/k1 (density ratio)
SHELL, MW 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
SHELL, LMC2 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
SHELL, SMC 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
DUSTY, MW 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
DUSTY, LMC2 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
DUSTY, SMC 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
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