- 26 Feb, 2018 4 commits
-
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
- 19 Feb, 2018 5 commits
-
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
- 16 Feb, 2018 6 commits
-
-
Médéric Boquien authored
-
Médéric Boquien authored
When using different line widths during a single run, ensure that the fluxes and other quantities are always computed correctly
-
Médéric Boquien authored
Ensure that the computation of the continuum level is correct when determining the equivalent width, in particular when the line width is very narrow.
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
- 15 Feb, 2018 1 commit
-
-
Médéric Boquien authored
-
- 25 Jan, 2018 4 commits
-
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
The formula from Sawicki et al. (2012) used to compute the χ² in the presence of upper limits was not correct. This led the χ² to depend directly on the absolute value of the upper limit. The formula has been rederived and corrected.
-
Médéric Boquien authored
-
- 15 Jan, 2018 1 commit
-
-
Médéric Boquien authored
Fν was computed by calculating Fλ and then converting to Fν, which led to typical differences in fluxes of typically 1-2% and a bit more for a handful of pathological filters. Now Fν is computed directly and a bit faster. At the same time rather than computing an effective wavelength (which was more a mean wavelength), we compute the pivot wavelength, which is more appropriate when converting between Fν and Fλ.
-
- 05 Jan, 2018 1 commit
-
-
Médéric Boquien authored
When computing the attenuation curve, the bump is now added so that its relative strength does not depend on δ.
-
- 22 Dec, 2017 1 commit
-
-
Médéric Boquien authored
-
- 11 Dec, 2017 1 commit
-
-
Médéric Boquien authored
For more reliability we now save the chi² by blocks. Otherwise it could lead to some crashes when there was more than 1 redshift.
-
- 27 Nov, 2017 2 commits
-
-
Médéric Boquien authored
-
Médéric Boquien authored
Ensure that we do not try to fit bands that have an error bar of 0 mJy. We now simply discard such bands.
-
- 05 Nov, 2017 1 commit
-
-
Médéric Boquien authored
-
- 01 Nov, 2017 1 commit
-
-
Médéric Boquien authored
-
- 31 Oct, 2017 3 commits
-
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
- 25 Oct, 2017 1 commit
-
-
Médéric Boquien authored
Change the way the Maraston models are built in order to capture the rapid evolutionary phases, similarly to the changes done for the BC03 models.
-
- 19 Oct, 2017 1 commit
-
-
Médéric Boquien authored
In order to capture short evolutionary phases we assume that over 1 Myr star formation occurs in 10 small episodes every 0.1 Myr, rather than 1 large episode every 1 Myr and nothing in-between.
-
- 18 Sep, 2017 6 commits
-
-
Médéric Boquien authored
Add the option to build the database with the high resolution BC03 models rather than the low resolution ones.
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
Médéric Boquien authored
-
- 20 Jul, 2017 1 commit
-
-
Médéric Boquien authored
-