Dust extinction curves: Ferrara (1999) original resolution

<p>These datasets are based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>, and are intended to closely match the models run by <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> - they use the same dust grain properties and galactic geometry. Additionally, they are tabulated at the same inclinations, optical depths, wavelengths, and morphologies as in <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a>.</p> <p><strong>Dust Properties</strong></p> <p>Dust grain albedos, scattering asymmetries, and opacities to extinction are taken from <a href="http://adsabs.harvard.edu/abs/1997ApJ...487..625G">Gordon et al. (1997)</a>, for either their Milky Way, &ldquo;MW&rdquo;, or Small Magellanic Cloud, &ldquo;SMC&rdquo;, models (as encoded in each file name), and assume Henyey-Greenstein scattering.</p> <p>&nbsp;</p> <p><strong>Stellar Geometry</strong></p> <p>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 <a href="http://adsabs.harvard.edu/abs/1983MNRAS.202..995J">Jaffe (1983)</a> profiles. Note that spheroid radii in this work are listed as the scale radius, <em>r</em>_s, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, <em>r</em>_e=<em>r</em>_s/1.16.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em>_z, of the stellar disk scale height. The value of <em>h</em>_z is encoded in each file name.</p>