Dust emission
For modeling dust emission, various components can be added.
The obvious parties are: big dust grains in thermal equilibrium,
PAH and small dust grains not in thermal equilibrium. For modeling
in the submm and beyond, perhaps there is emission from very
cold dust, and the synchrotron radiation can start playing a role.
These, along with the value of the total amount of light reprocessed
by dust, generate the galaxy SEDs in these wavelengths. The observed
color-luminosity relations can be used to constrain the modeling.
We also have more than 1,000 IR SEDs at z=0 inherited from
the WIRE modeling to compare with any of these models.
References page
Introduction page
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Fan Fang
Last update: 26-July-99