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--- data:data_analysis_manual [2024/11/11 20:28]
Peter Young [Line fitting]
+++ data:data_analysis_manual [2026/03/28 18:46] (current)
eric buchlin Fix link
@@ Line 236: / Line 236: @@
 Links:
+  * Python quicklook tool: [[https://pypi.org/project/spiceitup/|SPICE-IT-UP]].
   * Example with [[:data:data_analysis_manual:sunraster|with sunraster]].
   * Tutorial about [[https://git.ias.u-psud.fr/spice/data-analysis-club/-/blob/main/20230516-coordinates/coordinates.ipynb|plotting and coordinates transforms]]
@@ Line 263: / Line 264: @@
 ==== Line fitting ====
+For IDL Gaussian fitting software, please check: **[[data:line_fitting_idl|IDL software for emission line fitting]]**.
-=== Fitting a Gaussian at each spatial pixel in a raster (IDL) ===
+Fitting in Python can be done with any fitting library, including [[https://docs.astropy.org/en/stable/modeling/|astropy.modelling]]. From astropy 7.0, there is a user-friendly way of doing the fitting in parallel ([[https://github.com/aperiosoftware/parallel-modeling-examples/blob/main/spice/Final_Tutorial.ipynb|tutorial]] by Stuart Mumford).
-Spectra at each spatial pixel in a raster can be fit with Gaussians using the eis\_auto\_fit IDL routine developed for the Hinode/EIS mission (you must have the EIS branch in your Solarsoft distribution). The key step is to format a SPICE wavelength window into a "windata" structure using the routine spice\_getwindata. An example call is:
-''
-IDL> wd=spice\_getwindata(file)   ; choose a wavelength window \\
-IDL> eis\_fit\_template,wd,template  ; create a template for the fit\\
-IDL> eis\_auto\_fit,wd,fit,template=template\\
-IDL> eis\_fit\_viewer,wd,fit
-''
-The routine eis\_fit\_viewer is a GUI-based routine for browsing the fit results. More details on the eis\_auto\_fit suite of routines are available in [[https://doi.org/10.5281/zenodo.6339584
-|EIS Software Note 15]].
-The EIS software enable a number of operations to be performed on windata structures, as described in [[https://sohoftp.nascom.nasa.gov/solarsoft/hinode/eis/doc/eis_notes/21_WINDATA/eis_swnote_21.pdf|EIS Software Note 21]]. For example, eis\_bin\_windata allows spatial binning of the rasters.
-If you have problems running the EIS software on SPICE data, please contact [[https://science.gsfc.nasa.gov/sed/bio/peter.r.young|Dr. Peter Young]].
-=== Fitting a Gaussian to a spatially-averaged spectrum (IDL) ===
-In this scenario, a spatial region is selected in the raster, perhaps a bright point or a loop, and the spectra are averaged over this region to produce a single, 1D spectrum. Gaussians are then fit to this spectrum. The procedure is as follows:
-''
-IDL> map=spice\_make\_image(file,770.4)   ; for Ne VIII 770.4\\
-IDL> mask=pixel\_mask\_gui(map)   ; GUI routine for selecting pixel mask\\
-IDL> spec=spice\_mask\_spectrum(file,mask)   ; create averaged spectrum\\
-IDL> spec\_gauss\_spice, spec    ; GUI routine for fitting Gaussians
-''
-These routines are modified from routines originally written for Hinode/EIS. Further details can be found in [[https://doi.org/10.5281/zenodo.6339584
-|EIS Software Note 15]].
+This is used by the [[https://pypi.org/project/pycfit/|PyCFIT]] library, which provides a GUI for fitting the different components.
 === Line window width and spectral tilt ===

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