zmet distributed like P(Z) = exp(-z/z_mean), no age dependency.

Generates a model object with the current parameters.

Calculate the ratio A(lambda)/A(V) for the Calzetti et al. (2000) attenuation curve.

Generates a model object with the current parameters.

Thermally broadened frequency (in Hz), given a temperature `T` in K (see Dijkstra 2014) and optional turbulent velocity `b` in km/s

Fit the specified object and update the catalogue.

This function samples from a Dirichlet distribution based on N-1 independent random variables (r) in the range (0, 1). The method is that of

Calculates advanced derived posterior quantities, these are slower because they require the full model spectra.

Obtain a 1D spectrum for a given star-formation and chemical enrichment history, ionization parameter and t_bc. parameters -

Get the IGM transmission at a given redshift.

This method generates predictions for observed photometry. It resamples filter curves onto observed frame wavelengths and integrates

Calculate the ratio A(lambda)/A(V) for the Cardelli et al. (1989) extinction curve.

Interpolates a chosen grid in logU and collapses over star- formation and chemical enrichment history to get 1D models.

Calculate the ratio A(lambda)/A(V) for the Gordon et al. (2003) Small Magellanic Cloud extinction curve. Warning: this currently dive

Adds model photometry to the passed axis.

Adds photometric data to the passed axes.

Add a spectrum to the passed axes. Adds errors if they are included in the spectrum object as a third column.

Calculate IGM transmission using Inoue et al. (2014) model.

Makes a bagpipes burst model and returns the spectrum.

Calculates photometric fluxes. The filters are first re- sampled onto the same wavelength grid with transmission values blueshifted b

A general function for turning an array of bin midpoints into an array of bin left hand side positions and bin widths. Splits the distance be

Resamples the filter curves onto a new set of wavelengths and creates a 2D array of filter curves on this sampling.

Sample from the prior distribution.

Measure spectral indices, either an EW or flux ratio.

Update the model outputs to reflect new parameter values in the model_components dictionary. Note that only the changing of numerical

Two component dust law based on Charlot + Fall (2000) model, Stars still embedded in birth clouds (age < 10Myr) have steeper

Approximation of Voigt function of `x` (from Tasitsiomi 2006 or Tepper-Garcia 2006), given a temperature `T` in K and optional turbulent

Calculates effective wavelengths for each filter curve.

This method combines the models for the various emission and absorption processes to generate the internal full galaxy spectrum held

Finds the min and max wavelength values across all of the filter curves.

This method generates predictions for observed spectroscopy. It optionally applies a Gaussian velocity dispersion then resamples onto

Obtain (unnormalised) rest-frame UVJ magnitudes.

Convert between ergs s^-1 cm^-2 A^-1 and microjanskys if there is a difference between the specified input and output units.

Run through the catalogue fitting multiple objects at once on different cores.

Calculate wavelength sampling for the model to be resampled onto in order to apply variable spectral broadening. Only used if a resol

Generate an appropriate spec_wavs array for covering the spectral indices specified in index_list.

Calculate the optimal wavelength sampling for the model given the required resolution values specified in the config file. The way th

Calculates the log-likelihood for spectral indices.

Calculates the log-likelihood for spectral indices.

Calculates the log-likelihood for photometric data.

Calculates the log-likelihood for spectroscopic data. This includes options for fitting flexible spectral calibration and covariant n

Loads filter files for the specified filt_list and truncates any zeros from either of their edges.

Set the error spectrum to infinity in masked regions.

Print the 16th, 50th, 84th percentiles of the posterior.

Read MultiNest data. By default, Fortran drops the "E" symbol for 3-digit exponent output (e.g., '0.148232-104'). This impacts the outpu

Resamples the intermediate stellar grids to the age sampling which is set in the config file. This has to be done carefully as summin

Resamples the raw stellar grids to the input wavs.

Resample the raw grid to the input wavelengths.

Calculate constant factors used in the lnlike function.

Sets the corrrect redshift (range) in self.fit_instructions for the object being fitted.

Set up the initial blank output catalogue.

Loads Cloudy nebular continuum grid and resamples to the input wavelengths. Loads nebular line grids and adds line fluxes to the corr

Set up list of variables to go in the output catalogue.

Adds photometric data to the passed axes without doing any manipulation of the axes or labels.

Creates a plot of sfr(t) for a given star-formation history.

Delta function metallicity history, default unless specified.

Lyman-alpha optical depth given a neutral hydrogen column density `N_HI` in cm^-2, temperature `T` in K, and optional turbulent velocity

Loads individual cloudy results from the output files and converts the units to L_sol/A for continuum, L_sol for lines.

Run through the catalogue fitting each object. Parameters ---------- verbose : bool - optional Set to True to g

Calculates basic posterior quantities, these are fast as they are derived only from the SFH model, not the spectral model.

Calculates basic prior quantities, these are fast as they are derived only from the SFH model, not the spectral model.

Calculate tx vals for any Dirichlet distributed params.

Interpolates separately on both sides of a discontinuity, not over it

Obtain line fluxes for a given star-formation and chemical enrichment history, ionization parameter and t_bc. parameters ---

Returns the log-likelihood for a given parameter vector.

Makes an instructions file for cloudy.

Saves a bagpipes spectrum in the correct format to the cloudy sed files directory.

convert x and y arrays for a line plot to a histogram plot.

Combines array sections from different cores.

Distributes array elements to cores when using mpi.

Make a quick plot of the data loaded into a galaxy object.