Obtain posterior predictions for new observables not included in the data.

Run an individual cloudy model.

Lyman-alpha scattering cross section (e.g. Dijkstra 2014) given a temperature `T` in K and optional turbulent velocity `b` in km/s; note

Transform numbers on the unit cube to the prior volume.

Modified Charlot + Fall (2000) model of Carnall et al. (2018) and Carnall et al. (2019b).

A GP noise model that uses celerite2's SHOTerm kernel for corellated noise and white noise (jitter term). This have been show

A GP noise model including a double exponenetial squared kernel for corellated noise and white noise (jitter term).

A GP noise model including an exponenetial squared kernel for corellated noise and white noise (jitter term).

Gaussian prior between limits with specified mu and sigma.

A delta function burst of star-formation.

constant metallicity without any variation in time, distribution of coeval stars can be specified thorugh 'metallicity_scatter'

Constant star-formation between some limits.

Bayesian fitting of Chebyshev calibration polynomial.

Exponential prior in x where x is the parameter.

Fit the specified model to the input galaxy data. Parameters ---------- verbose : bool - optional Set to True t

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

Uniform prior in log_10(x) where x is the parameter.

Uniform prior in log_e(x) where x is the parameter.

log normal metallicity distribution for coeval stars. Functional form: P(x) = 1/(x*sigma*np.sqrt(2*np.pi)) * n

Equations for finding the tau and T0 for a lognormal SFH given some tmax and FWHM. Needed to transform variables.

Make local Bagpipes directory structure in working dir.

Make up the igm absorption table used by bagpipes.

Different metallicities in each specificed time bin.

Work like Leja continuity SFH, zmet varies with dirichlet prior.

Plot the posterior of the calibration spectral correction.

Make a corner plot of the fitted parameters.

Make a quick plot of an individual model galaxy.

Make a quick plot of an individual model galaxy.

Make a quick plot of an individual sfh.

Make a plot of the SFH posterior.

Plot the observational data and posterior from a fit object.

Bayesian fitting of Chebyshev calibration polynomial.

Uniform prior in 10**x where x is the parameter.

Predicts basic (SFH-based) quantities at a specified higher redshift. This is a bit experimental, there's probably a better way. Only

2-step metallicities (time-varying!) for psb_wild2020 SFH model shift in metallicity at burstage parameter from SFH model For

A 2-component SFH for post-starburst galaxies. An exponential compoent represents the existing stellar population before the

Uniform prior in 1/x**2 where x is the parameter.

Generate the whole grid of cloudy models and save to file.

Obtain a split 1D spectrum for a given star-formation and chemical enrichment history, one for ages lower than t_bc, one for ages hig

Get the 1D spectrum for a given set of model parameters.

Test the above code by generating a plot from Inoue et al. (2014).

2-step metallicities (time-varying!) time of shift is a free parameter

Uniform prior in x where x is the parameter.

A simple variable noise model with no covariances. Scales the input error spectrum by a constant factor.