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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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**A description of identification and classification of HCO+ baseline fitting issues in the TP data (SPW 21)**
**Identification:** Baseline issues can be identified in plots from the HSD_Baseline t…
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This is driven by astropy/specutils#303. When fitting spectral lines, we want to know which parameter of a model is the "center". In `specutils` the planned solution for now is to just guess based o…
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**Describe the bug**
Executing the example positionswitch I get this warning when a baseline fit is done
WARNING: The fit may be poorly conditioned [astropy.modeling.fitting]
Perhap…
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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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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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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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The toolbox as we have demonstrated it is set up for spectral rendering. For some applications, features of the render toolbox may be highly useful, but spectral rendering will not be needed. The use …
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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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### 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/_…