Making model spectra: model_galaxy¶
Model galaxy spectra and associated observables are created using the
model_galaxy class. Check out the first iPython notebook example for a quick-start guide to making models.
model_galaxy(model_components, filt_list=None, spec_wavs=None, spec_units='ergscma', phot_units='ergscma', index_list=None)¶
Builds model galaxy spectra and calculates predictions for spectroscopic and photometric observables.
- model_components (dict) – A dictionary containing information about the model you wish to generate.
- filt_list (list - optional) – A list of paths to filter curve files, which should contain a column of wavelengths in angstroms followed by a column of transmitted fraction values. Only required if photometric output is desired.
- spec_wavs (array - optional) – An array of wavelengths at which spectral fluxes should be returned. Only required of spectroscopic output is desired.
- spec_units (str - optional) – The units the output spectrum will be returned in. Default is “ergscma” for ergs per second per centimetre squared per angstrom, can also be set to “mujy” for microjanskys.
- phot_units (str - optional) – The units the output spectrum will be returned in. Default is “ergscma” for ergs per second per centimetre squared per angstrom, can also be set to “mujy” for microjanskys.
- index_list (list - optional) – list of dicts containining definitions for spectral indices.
Update the model outputs to reflect new parameter values in the model_components dictionary. Note that only the changing of numerical values is supported.
The model_components dictionary¶
The first and most important argument passed to
model_galaxy is the
model_components dictionary. This contains all of the physical information about the model you wish to create. A complete guide to the
model_components dictionary is provided here.
Getting observables - photometry¶
In order to obtain predictions for photometric observations of a galaxy with the physical parameters defined in
model_components it is necessary to define a list of filter curves through which observed fluxes should be calculated. This is done by defining a
This is simply a list of paths (absolute or from the directory in which the code is being run) to the locations at which these filter curves are stored. The filter curve files should contain wavelengths in Angstroms in their first column and relative transmission values in their second.
Let’s look at a simple example of some code which creates predictions for photometry through a series of filter curves. For this to work you’d first need to put the filter curve files in the correct location. For sourcing filter curves I recommed the SVO Filter Profile Service.
import bagpipes as pipes import numpy as np uvista_filt_list = ["uvista/CFHT_u.txt", "uvista/CFHT_g.txt", "uvista/CFHT_r.txt", "uvista/CFHT_i+i2.txt", "uvista/CFHT_z.txt", "uvista/subaru_z", "uvista/VISTA_Y.txt", "uvista/VISTA_J.txt", "uvista/VISTA_H.txt", "uvista/VISTA_Ks.txt", "uvista/IRAC1", "uvista/IRAC2"] model = pipes.model_galaxy(model_components, filt_list=uvista_filt_list) model.plot()
We now have a Bagpipes model galaxy! The final command generates a plot of the predicted fluxes.
Photometry is accessible as
model.photometry, which is a 1D array of flux values in erg/s/cm^2/A in the same order as the filter curves are specified in
filt_list. The output flux units can be converted to microJanskys using the
model_galaxy keyword argument
Getting observables - spectroscopy¶
The process for obtaining model spectroscopy is simpler, just pass an array containing the desired wavelength sampling in Angstroms as the
spec_wavs keyword argument.
import bagpipes as pipes import numpy as np obs_wavs = np.arange(2500., 7500., 5.) model = pipes.model_galaxy(model_components, spec_wavs=obs_wavs) model.plot()
The output spectrum is stored as
model.spectrum which is a two column array, containing wavelengths in Angstroms and spectral fluxes in erg/s/cm^2/A by default. The output flux units can be converted to microJanskys using the
model_galaxy keyword argument
Getting observables - line fluxes¶
Emission line fluxes are stored in the
model_galaxy.line_fluxes dictionary. The list of emission features is here. These are only non-zero if a
nebular component is added to
Emission line naming conventions are the same as in Cloudy. The names in the above file are the keys for the lines in
model_galaxy.line_fluxes. For example, the Lyman alpha flux is under:
model.line_fluxes["H 1 1215.67A"]
Emission line fluxes are returned in units of erg/s/cm^2.
Note on units at redshift zero¶
The units specified above apply at non-zero redshift, however at redshift zero the luminosity distance is zero which would lead to a division by zero error. At redshift zero the code instead returns luminosities, in erg/s/A for spectroscopy and photometry, and erg/s for emission lines.
Creating a new
model_galaxy is relatively slow, however changing parameter values in
model_components and calling the
update method of
model_galaxy rapidly updates the output predictions described above.
It should be noted that the
update method is designed to deal with changing numerical parameter values, not with adding or removing components of the model or changing non-numerical values such as the dust attenuation type.