Start the parallel processes with fork rather than spawn on Linux platforms, resulting in a faster startup.

Add the possibility to have an exponential burst with the sfhdelayed module in order to model the latest episode of star formation.

When using different line widths during a single run, ensure that the fluxes and other quantities are always computed correctly

Ensure that the computation of the continuum level is correct when determining the equivalent width, in particular when the line width is very narrow.

The formula from Sawicki et al. (2012) used to compute the χ² in the presence of upper limits was not correct. This led the χ² to depend directly on the absolute value of the upper limit. The formula has been rederived and corrected.

Fν was computed by calculating Fλ and then converting to Fν, which led to typical differences in fluxes of typically 1-2% and a bit more for a handful of pathological filters. Now Fν is computed directly and a bit faster. At the same time rather than computing an effective wavelength (which was more a mean wavelength), we compute the pivot wavelength, which is more appropriate when converting between Fν and Fλ.

When computing the attenuation curve, the bump is now added so that its relative strength does not depend on δ.

Ensure that we do not try to fit bands that have an error bar of 0 mJy. We now simply discard such bands.

In order to capture short evolutionary phases we assume that over 1 Myr star formation occurs in 10 small episodes every 0.1 Myr, rather than 1 large episode every 1 Myr and nothing in-between.

Add the option to build the database with the high resolution BC03 models rather than the low resolution ones.

The computation of the fit taking into the upper limits would only work for the first few models because the number of bands was taken as the number of models.

Read the list of sed modules from pcigale.ini. This is more flexible than inferring this list from the input parameters file as some modules can be missing (for instance when using the default values for all the parameters of a given module).

Compute the best fit at the at the exact distance of the analysed object and not at the distance of the rounded redshift. This eliminates the need for a correction factor.

Implement an observations manager. For now it is mainly used as a simple container for the observations table but upcoming rearchitecturing will make full use of it.