- 19 Feb, 2018 5 commits
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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- 16 Feb, 2018 6 commits
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Médéric Boquien authored
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Médéric Boquien authored
When using different line widths during a single run, ensure that the fluxes and other quantities are always computed correctly
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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.
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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- 15 Feb, 2018 1 commit
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Médéric Boquien authored
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- 25 Jan, 2018 4 commits
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Médéric Boquien authored
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Médéric Boquien authored
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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.
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Médéric Boquien authored
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- 15 Jan, 2018 1 commit
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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.
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- 05 Jan, 2018 1 commit
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Médéric Boquien authored
When computing the attenuation curve, the bump is now added so that its relative strength does not depend on δ.
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- 22 Dec, 2017 1 commit
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Médéric Boquien authored
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- 11 Dec, 2017 1 commit
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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.
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- 27 Nov, 2017 2 commits
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Médéric Boquien authored
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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.
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- 05 Nov, 2017 1 commit
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Médéric Boquien authored
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- 01 Nov, 2017 1 commit
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Médéric Boquien authored
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- 31 Oct, 2017 3 commits
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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- 25 Oct, 2017 1 commit
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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.
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- 19 Oct, 2017 1 commit
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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.
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- 18 Sep, 2017 6 commits
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Médéric Boquien authored
Add the option to build the database with the high resolution BC03 models rather than the low resolution ones.
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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Médéric Boquien authored
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- 20 Jul, 2017 1 commit
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Médéric Boquien authored
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- 02 May, 2017 1 commit
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Médéric Boquien authored
The computation of the fit taking into the upper limits would only work for the first few models because the number of bands was taken as the number of models.
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- 14 Apr, 2017 1 commit
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Médéric Boquien authored
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- 10 Apr, 2017 2 commits
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Médéric Boquien authored
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Médéric Boquien authored
The standardisation of error bars must be done on the final estimates, not on the estimates for a single block.
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