Emission models¶
Overview¶
To simplify the calculation of complex emission, with many contributing components and different operations involved in their construction, Synthesizer provides EmissionModels.
At their simplest, EmissionModels define a set of inputs and produce an emission (spectra or emission lines), e.g. the incident emission from a stellar component based on an SPS Grid.
However, EmissionModels can be arbitrarily complex, defining multiple different types of spectra and lines from different components, and defining how they interact.
The possible operations that EmissionModels can define are:
Extraction of an emission from a
Grid(see the Emission model basics).Generation of SED or line from stars or AGN (see Stellar and AGN Models in), including the addition of dust emission (dust emission docs) or AGN torus emission (AGN models docs)
Transformation of an emission, e.g. applying a dust curve (see the dust attenuation docs) or IGM attenuation (see the IGM attenuation docs).
Combination of spectra.
Any of these operations can be done in the presence of a property mask, to apply the operation to a subset of the components contents (e.g. applying dust attenuation only to young stars), or a wavelength mask to apply the operation only to a subset of the wavelength range. These masks can be applied identically to particle or parametric models.
Once an EmissionModel is constructed it can be used to generate spectra.
This is done by passing the EmissionMmodel to the get_spectra or get_lines method on a Galaxy or galaxy component.
This will then generate the spectra defined within the EmissionModel, given the properties of the Galaxy or component.
For more details for manipulating these, see Galaxy spectra, Stellar spectra or Blackhole spectra.
Working with EmissionModels¶
In the sections linked below we detail the basic functionality of an EmissionModel, the premade stellar and black hole emission models, dust emission generators, and how to customise a model or construct your own.