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The normalization of the global covariance is described by a free parameter `logAmp` (the actual normalization is `(10**logAmp)**2`). But if such normalization is much higher than the median value of …
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In my research, modelling the line spread function (LSF) of the data is important when I am degrading synthetic stellar spectra to the observed data quality to measure stellar parameters. Many spectra…
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**Gammapy version**
1.0.1
**Bug description**
LightCurveEstimator fails when I set Reoptimize = True (it works with it as False), saying my model has no free parameters (but amplitude is free).
…
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_Discussed with Akpona and Neija._
It is proposed to implement an algorithm that calculates an indicator for band noisiness, e.g. mean residuals of fitted versus original data.
This should identify …
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Several searches use 1D spectral fits, binned or unbinned.
They use sometimes functional forms for background/signals, and sometimes templates.
It would be great to make a general class for these …
kdund updated
9 months ago
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This tackles a subset of the points raised in #81 where we define the format of the instrument data to be fitted.
The aim is to ensure that the loading of the data and creation of the spectrum t…
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Copied over from fooof-tools/fooof#124, original post by @rdgao with comments by @parenthetical-e :
Currently, peaks are identified based on a combination of user-defined threshold and comparison t…
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Sgr_A_st_v_03_TP
[uid://A001/X15a0/X122](https://almascience.org/aq/?result_view=observation&mous=uid://A001/X15a0/X122)
* [x] Observations completed?
* [x] Delivered?
* [x] Downloaded? (specify whe…
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### Describe the workflow you want to enable
Save the spectral embeddings used for clustering in the [SpectralClustering](https://github.com/scikit-learn/scikit-learn/blob/9aaed4987/sklearn/cluster/_…