DIRTY Spherical Galacitic Environment Data

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These model runs use the Clayton et al. (2003) dust grain models for MW, LMC2, and SMC dust. They also cover a wider range of wavelengths (0.08 - 1000 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.

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
CLOUDY, MW 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
CLOUDY, LMC2 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
CLOUDY, SMC 1.000 (homogeneous) 0.500 0.100 0.050 0.010 (clumpy) 0.005 0.001
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