Now that we do not add an AGN component anymore when the AGN fraction is 0, the wavelength grid may change from one model to the other. To work around this issue we save the IGM component into a dictionary with the key being the size of the grid. This is not completely foolproof as two grids of same length may have different wavelengths, though that is quite unlikely given pcigale's architecture. It should be good enough for now.

If the AGN fraction is 0, then there is no need to add a component to the SED. It would have a value of 0 everywhere. It looks like we gain around 30% in computation time in this case.

Computing the luminosity each time we integrate in a filter (for instance) is not efficient. As the luminosity is in effect modified in only one place (add_contribution), let's just compute it manually each we add a component. This yields a ~10% improvement.

Update the Dale 2014 model with a finer sampling. We now use the same grid as the Draine models. Courtesy Daniel Dale.

In the Bruzual and Charlot (2003) SSP module, we add parameters to the
info dictionary containing the total star and gas masses for the galaxy.

Specify that encoding for pcigale.ini. Otherwise if a non-ASCII character is used it may work or crash depending on the computer. Now we encode everything in UTF-8, which will allow again to use these chracters in the description of the modules parameters.

Use the base numpy interp() function rather than scipy's interp1d(). The reason is that when interpolation only 1 array the former is much faster (probably because it is compiled and there is no overhead returning a function. We can only do that for the new component. For the old ones, there are too many for this to be worthwhile. Still, it nets a nice improvement.

The wavelength arrays are sorted. So there is no need to call min() and max() to find the extrema. We can directly get the first and last elements.

Small optimisation in the interpolation. There is no need to sort the arrays because they are already sorted.

Add errorbars to the SED plots. Because they tend to be small compared to the dynamic range, we use 3σ uncertainties rather than just 1σ.

Build the BC03 models only up to 14 Gyr rather than 20 Gyr. The use case for 20 Gyr is very weak. Limiting to 14 Gyr brings two major advantages: it reduces the size of the database from 3.6GB to 2.9GB and it should make the computation faster as the SSP grid size is smaller.