- The (1+z1)/(1+z2) factor between observed and grid flux densities caused by the differential redshifting is now taken into account. With a default grid redshift rounding of two decimals this yields a difference of at most 0.5% in the estimated physical properties at z=0 and even less at higher z. (Médéric Boquien)
- The list of bands for which to carry out a Bayesian flux estimate is now configurable. By default this corresponds to the fitted bands but it also supports bands that are not included in the fit. This can be set in the `fluxes` parameter of the `pdf\_analysis` module. (Médéric Boquien)
- Implementation of the auto-detection of lines in the input flux file so they are automatically added to the list of bands in `pcigale.ini`. (Médéric Boquien)
- The `dl2007` and `dl2014` modules now provide \<U\>. (Médéric Boquien)
- Saving the χ² is now a bit more fine-grained. It is possible to save none, all, only the properties, or only the fluxes. (Médéric Boquien)
- The database now includes the JWST MIRI and NIRCam filters. (Médéric Boquien)
### Changed
- Python 3.6 is now the minimum required version. (Médéric Boquien)
- The logo has now been moved to the lower-right corner of the figure so that it does not overlap with any information and it has been updated for a less pixelated version. (Médéric Boquien & Rodrigo González Castillo)
- The wavelength range in SED plots is now dynamically adapted to cover the observed wavelengths. (Médéric Boquien)
- The uncertainties on the SED plots now correspond only to 1σ rather than 3σ so they do not appear exceedingly large. (Médéric Boquien)
- The lines linking the different bands in the residual SED plot have been eliminated to improve the readability. (Médéric Boquien)
- Some lines have been made slightly thicker in SED plots so the different components are more visible. (Médéric Boquien)
- The colours in the SED plots have been tweaked for aesthetic reasons. (Médéric Boquien)
- The markers for the observed fluxes in the SED plots have been tweaked to improve readability. (Médéric Boquien)
- The computation of all the cosmology-dependent quantities has been consolidated in pcigale/utils/cosmology.py and optimised. This leads to a slightly faster startup, in particular when there are many objects to fit, and it makes it easier to change the cosmology. (Médéric Boquien)
- The time spent computing is now displayed in hours, minutes, and seconds rather than just seconds to improve legibility. (Médéric Boquien)
### Fixed
- Make sure we can plot the PDF of equivalent widths. (Médéric Boquien)
- Fix a crash when generating a mock catalogue containing intensive properties. (Médéric Boquien)
...
...
@@ -13,8 +28,18 @@
- Fix the pip install by making pcigale.managers discoverable. (Yannick Roehlly)
- When using a parameters file, Boolean values were not correctly interpreted. (Médéric Boquien, reported by Eric Martínez, INAOE)
- Make sure that the best-fit models are stored with the correct scaling factor when the distance is given explicitly (Médéric Boquien)
- Some labels and the title for the SED plots has been improved to avoid overlaps and overflows. (Médéric Boquien)
- Ensure that best models are properly computed when models are computed by blocks and that no fit could be made in one or more blocks. This can be case if all the models in the block are older than the age of the universe. (Médéric)
- Make sure that the parameters are saved with the proper scale (linear or logarithmic) in the χ² files. (Médéric Boquien)
- Some math libraries such as MKL or OpenBLAS sometime try to be (too) smart, starting computation threads on their own. As cigale is already parallel, this just oversubscribes the CPU and can lead to important slowdowns. An environment variable could be set by the user to disable this, but this is cumbersome. Rather, we set these variables directly in the code at the startup of cigale. (Yannick Roehlly & Médéric Boquien)
### Optimised
- Slight speedup of the computation of the likelihood from the χ² (Médéric Boquien)
- Slight speedup of the computation of the likelihood from the χ² using a multiplication rather than a division. (Médéric Boquien)
- Speedup of the computation of the χ² by ~10% taking the opposite of a scalar rather than of an array. (Médéric Boquien)
- Thanks to a change in the layout of the models storage in RAM, the computation of the χ² is now massively faster when the run contains multiple redshifts. (Médéric Boquien)
- The computation of the weighted means and standard deviations has been made ~50% faster by normalising the likelihood. (Médéric Boquien)
- The the fritz2006 module should now run faster thanks to an optimisation of the computation of the luminosity of the various AGN components (Médéric Boquien & Guang Yang)
- Various optimisations have been made regarding shared arrays to make their access faster. The overall effect is a speedup of 3-4% for the computation of the models. (Médéric Boquien)
- All the cores should now be used over the entire duration of the computation of the Bayesian and best-fit estimates. Before the number of active cores could drop towards the end of the computation. (Médéric Boquien)
# Includes Nominal transmission of the JWST OTE is not included. Source: http://svo2.cab.inta-csic.es/svo/theory/fps3/index.php?mode=browse&gname=JWST&gname2=MIRI
# Includes Nominal transmission of the JWST OTE is not included. Source: http://svo2.cab.inta-csic.es/svo/theory/fps3/index.php?mode=browse&gname=JWST&gname2=MIRI
