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.

As we loop over the bands to compute the χ², it is smarter that the bands are the slower varying index and the models the faster varying index. That way it is more likely that models at the correct redshift are prefetched into the cache.

Use a multiplication rather than a division to convert luminosities into fluxes. This should yield a small speedup.

When giving the list of parameters through a file, cigale did not compute properly what parameter changed between to successive models.

With the new sanity check of the input parameters, cigale did not handle the fact that the redshift could be given in the parameters file. Now this is handled properly.

A significant fraction of the total run time is spent computing integrals (e.g. fluxes in passbands). We can make the integration faster by rewriting the trapezoidal rule in terms of np.dot(). This allows to offload the computation to optimised libraries. The end result is that the integration is twice as fast, with a gain of ~10-15% on the total run time.

0.9.0 release

Samuel Boissier gave us extended values down to a velocity of 40 km/s as well as
intermediate values for the SFH module sfh_buat08.

Convert individually each item of the input list as doing so on an the entire array generates an error if the expected type is int and the provided values are in floats.

Computers are much better at multiplying than at dividing. Therefore to correct the emission for redshifting we multiply by 1/(1+z) rather than dividing by 1+z.

The absorption of the Lyman continuum from old stars tended to be overestimated leading to some “negative fluxes” for the Lyman continuum.

In rare circumstances requiring a specific distribution of redshifts the integration of the spectrum in some filters was not done correctly, inducing relative errors of ~10¯⁵-10¯⁶.

To compute the stellar spectrum of the young component, do not pass the full SFH with the old part set to 0. Rather, only pass the corresponding part of the SFH. This nearly doubles the computing speed of the stellar spectrum.

We do not store the time grid in the SED anymore given that we assume it starts at 0 Myr with steps of 1 Myr, we can easily reconstruct to save it if needed. It should save a little bit of memory and it should go a little bit faster.

In the output the sfh.age parameter would correspond to the input value minus 1. Now both values are consistent with one another.