GitLab

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

In order to release a new version correcting some bugs, we remove the
work in progress correction for upper limits.

Correct the function adjusting the data and implements a new way to indicate
upper limits.

FIXME: This breaks other parts of the code that must be corrected because now
upper limits are indicated with a negative flux.

The test fails so that we can correct the function.

Rename (and correct a bug into) the SFH quenching module to sfh_quenching_trunk
and add a sfh_quenching_smooth version where the SFR is linearly decreasing
after the quenching.

The WFCAM Ks filter does not exist.
The filters J, and Y were wrong.
Add H, K, and Z filters.

Use a more human-friendly format for the ASCII output of savefluxes to facilitate visual inspection as a FITS output is now available for machine reading.

When on a grid, make sure that the models are always computed in the same order to facilitate comparisons between different runs.

Remove the output_file and output_format parameters from the savefluxes module. Now results are systematically saved as ASCII and FITS tables.

Clarify that if the parameters are given through a file, then the pdf_analysis module should not be used.

Correct the description of the radio module. It stated erroneously that it handled thermal emission whereas this is done by the nebular module.