Kim, Martin, and Hendry (1994) dust with Henyey-Greenstein scattering

These are dust properties from Kim, Martin, and Hendry (1994), also known as KMH. The dust consists of astronomical silicates, graphite, and carbon and the size distribution was determined using a maximum entropy method. This dust type is meant to be applicable to the diffuse ISM (for low column densities) in the Galaxy.


The dust properties given here are given per unit mass of gas+dust, assuming a gas-to-dust ratio of 141.84. This means that when using Hyperion, the total gas+dust densities should be specified.

This version of the dust file is take directly from HOCHUNK, the radiative transfer code developed by B. Whitney et al. This is the dust you should use if you want to reproduce results from that code, and it approximates the scattering with a Henyey-Greenstein function. However, if you are interested in the best version of the KMH dust, with full scattering properties, you can find this under Kim, Martin, and Hendry (1994) dust with full scattering properties.

The dust file is available in the hyperion-dust directory as dust_files/kmh94_3.1_hg.hdf5 (once you have run python build_dust).

Rv=3.1 (dust_files/kmh94_3.1_hg.hdf5)

The following plot gives an overview of the dust properties (as described in Preparing dust properties):