GitLab

According to the 2MASS paper the filters can be directly applied to spectra un Fλ. Despite the confusing mention that they are photon-counting, this means that they are actually in energy units.

Fix a crash in the computation of the χ² because previous optimisations had been been not fully propagated to the case of upper limits.

Give a more reasonable amplitude for the UV bump with dustatt_powerlaw. Otherwise it is a factor Rv too large compared to dustatt_calzleit.

Do not store anymore the filter type as all the filters are now assumed to be in units of energy. The conversion from photon to energy is carried out by the import procedure as needed.

Add the new restframe_param module. It replaces most of the functionality provided in the unofficial param module, which has been trimmed down to only computing fluxes in the observed frame and has been renamed fluxes. Unlike param, the restframe_param module is to be called before the redshifting module.

When calling np.sum(), the axis should be an integer, not a float, otherwise it triggers a very disgracious Numpy warning. Now it is gone.

Use np.take() rather than fancy indexing on large arrays. This accelerates the computation of the models by 10%.

Optimise the interpolation of the luminosity components 1. computing the interpolation of all the components in one step rather than interpolating separately for each component, and 2. caching some intermediate computations that only depend on the grid sampling and therefore apply to all physical components.

Speed up the computation of the models using the compiled interp function rather than the regular numpy one so we bypass checks on the size and type of the arrays.

Update the nebular models from Akio Inoue. Now log U is sampled in steps of 0.1 dex down to -4. Also deviations from the 10000K case B assumption are taken into account.

Limit the number of threads to 1 per process in order to prevent MKL from creating numerous threads leading to a strong oversubscription of the CPU/RAM as pcigale already does its own parallelisation.

Implement the computation of the mass-weighted age for the bc03 and m2005 module. This is done in the corresponding convolve() functions. The information is returned in a new variable called info_all, which also contains all the information when the entire SFH is included (rather than separating old and young populations).

Rather than calling convolve() twice, call it just once with the separation age as an argument et let it do the various different convolutions. While this is functionally equivalent, this allows to pass the full SFH to convolve(), which in turn is necessary to compute additional quantities. This patch is a preparatory work for the the implementation of mass-weighted ages.

Do not return the break strengths in the bc03 module as they are not computed corrected by a convolvution.

There is no need to return the wavelength grid after convolution in the data bc03 module, it is readily available in the bc03 sed module.

Homogenise the bc03 and m2005 data modules so they use the same variable names as far as possible. Comments have also been corrected and made consistent.

Version 0.10.0