THEMIS grids
The extinction (EXT_xx.RES files) and emission (SED_xx.RES files) spectra were computed with the DustEM numerical tool using the Mathis et al. (1983) radiation field, scaled by the factor G0 ∈ [0.1, 100]. The spectra are given on a grid containing 800 steps between 0.04 and 105 μm.
The emission files contain the the emission per proton for each grain population 4πνIν/NH in erg/s/H as a function of wavelength (NH is the proton column density). The grain populations are labelled with the following names:
- CM20: carbonaceous grains as defined in Jones et al. (2013). Grains up to 20 nm consist purely of aromatic-rich H-poor amorphous carbon, a-C, whereas bigger grains have a core/mantle structure, where the core is made of aliphatic-rich H-rich carbon, a-C:H, and the mantle of a-C with a thickness of 20 nm,
- aOlM5 + aPyM5: silicates as defined in Koehler et al. (2014). These core/mantle grains consist of amorphous silicate cores (olivine and pyroxene-normative composition, Mg-rich) and 5 nm mantles of a-C.
The extinction files contain the extinction cross-section (σabs+σsca) for each grain population per gram of dust type. The total optical depth and extinction are then (see the DustEM userguide):
τ(λ) = ∑tt (σabstt+σscatt) Mtt/MH mH NH
Aλ = 1.086 × τ(λ).
The size distribution files (SDIST_xx.RES) were also computed with DustEM and contain the mass distribution (a3 dn/dlna in cm3/H) as a function of the effective grain radius a in microns.
CM grains
♣ CM extinction spectrum → here
♣ CM emission spectrum for G0 = 1 → here
♣ CM temperature distribution for G0 = 1 → here
♣ CM size distribution → here
♣ CM emission spectra for G0 ∈ [0.1, 100] → here
CMM grains
Coming soon!
AMM grains
Coming soon!
AMMI grains
Coming soon!