Dust extinction curves: Ferrara (1999) high resolution

These datasets are based on the models described in Benson (2018), and are intended to closely match the models run by Ferrara et al. (1999) - they use the same dust grain properties and galactic geometry. However, they are tabulated using a much higher resolution grid of inclinations, optical depths, wavelengths, and morphologies than in Ferrara et al. (1999).

Dust Properties

Dust grain albedos, scattering asymmetries, and opacities to extinction are taken from Gordon et al. (1997), for either their Milky Way, “MW”, or Small Magellanic Cloud, “SMC”, models (as encoded in each file name), and assume Henyey-Greenstein scattering.

Stellar Geometry

Galactic disks follow exponential profiles in both radial and vertical directions, with the vertical scale height equal to 0.0875 times the radial scale length. Spheroids follow spherical Jaffe (1983) profiles. Note that spheroid radii in this work are listed as the scale radius, rs, while Ferrara et al. (1999) listed the corresponding effective radius, re=rs/1.16.

Dust Geometry

Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale height. The value of hz is encoded in each file name.