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--- data:data_analysis_manual [2024/11/11 19:17] – [Line fitting] Peter Young
+++ data:data_analysis_manual [2026/08/24 14:48] (current) – [Find data] added event list links Peter Young
@@ Line 22: / Line 22: @@
 The data levels, FITS files, and headers are described in
-  * The [[https://spice-wiki.ias.u-psud.fr/lib/exe/fetch.php/public:spice-uio-dpdd-0002-2.1-data_product_description_document_spicefits_.pdf|Data Products Description Document]] (DPDD)
+  * The {{ :public:spice-uio-dpdd-0002-2.2-data_product_description_document_spicefits_all_accepted.pdf |Data Product Description Document (DPDD) version 2.2}}
   * The LLDPDD for the Low-Latency (LL) files
@@ Line 88: / Line 88: @@
   * Accessible through IDL/SSW and Python/Fido
   * FIXME As of 2024-03-29, the SPICE files on VSO are old files from release 3.0 only
+Event lists:
+  * [[public:eventlists:flares|Flares]]
+  * [[public:eventlists:prominences|Prominences]]
 ===== Tips and Advice on Analyzing SPICE Data =====
@@ Line 236: / Line 240: @@
 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 268: @@
 ==== 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]].
+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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