Generate a star formation history. Parameters ---------- model_components : dict A dictionary containing information about the

Builds model galaxy spectra and calculates predictions for spectroscopic and photometric observables. Parameters ---------- model_c

Allows access to and maniuplation of dust attenuation models. This class calculates the absolute attenuation curve (A_lam/A_V) for the specif

Contains a model which is to be fitted to observational data. Parameters ---------- galaxy : bagpipes.galaxy A galaxy object co

A class for modelling the noise properties of spectroscopic data, including correlated noise. Parameters ---------- noise_dict : di

Provides access to the outputs from fitting models to data and calculating posterior predictions for derived parameters (e.g. for star-format

A class which allows for samples to be drawn from a joint prior distribution in several parameters and for transformations from the unit cube

A basic rest-optical AGN continuum + broad line model. Parameters ---------- wavelengths : np.ndarray 1D array of wavelength va

A class for modelling spectrophotometric calibration. Parameters ---------- calib_dict : dictionary Contains the desired parame

Allows access to and maniuplation of the dust emission models of Draine + Li (2007). Currently very simple, possibly could be sped up in some

Top-level class for fitting models to observational data. Interfaces with MultiNest or nautilus to sample from the posterior distributio

A container for observational data loaded into Bagpipes. Parameters ---------- ID : str string denoting the ID of the object to

Allows access to and maniuplation of the IGM attenuation models of Inoue (2014). Parameters ---------- wavelengths : np.ndarray

Allows access to and maniuplation of nebular emission models. These must be pre-computed using Cloudy and the relevant set of stellar emissio

Allows access to and maniuplation of stellar emission models. Parameters ---------- wavelengths : np.ndarray 1D array of wavele

Class for loading and manipulating sets of filter curves. This is where integration over filter curves to get photometry happens. Parameters

Fit a model to a catalogue of galaxies. Parameters ---------- IDs : list A list of ID numbers for galaxies in the catalogue